Aeolis Research | Publications 2022-2023

2023

Title:	Investigating Diurnal and Seasonal Turbulence Variations of the Martian Atmosphere Using a Spectral Approach
Authors:	Murdoch, Naomi; Stott, Alexander E.; Mimoun, David; Pinot, Baptiste; Chatain, Audrey; Spiga, Aymeric; Temel, Orkun; Garcia, Jorge Pla; Onodera, Keisuke; Lorenz, Ralph; Gillier, Martin; Newman, Claire; Garcia, Raphael F.; Lange, Lucas; Banfield, Don
Affiliation:	AA(Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France), AB(Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France), AC(Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France), AD(Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France), AE(Departamento de Física Aplicada, Escuela de Ingeniería de Bilbao, Universidad del País Vasco/Euskal Herriko Unibertsitatea (UPV/EHU), Bilbao, Spain), AF(Laboratoire de Météorologie Dynamique/Institut Pierre Simon Laplace (LMD/IPSL), Sorbonne Université, Centre National de la Recherche Scientifique (CNRS), École Polytechnique, École Normale Supérieure (ENS), Paris, France; Institut Universitaire de France, Paris, France), AG(KU Leuven, Institute of Astronomy, Leuven, Belgium; Royal Observatory of Belgium, Reference Systems and Planetology, Brussels, Belgium), AH(Centro de Astrobiología, (CSIC-INTA), Madrid, Spain), AI(Earthquake Research Institute, The University of Tokyo, Tokyo, Japan), AJ(Johns Hopkins Applied Physics Laboratory, 11100 Johns Hopkins Road, Laurel, MD, 20723, USA), AK(Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France), AL(Aeolis Research, Chandler, AZ, USA), AM(Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France), AN(Laboratoire de Météorologie Dynamique/Institut Pierre Simon Laplace (LMD/IPSL), Sorbonne Université, Centre National de la Recherche Scientifique (CNRS), École Polytechnique, École Normale Supérieure (ENS), Paris, France), AO(NASA Ames, Mountain View, CA, USA)
Journal:	The Planetary Science Journal, Volume 4, Issue 11, id.222, <NUMPAGES>18</NUMPAGES> pp.
Publication Date:	Nov 2023
Origin:	American Astronomical Society
Keywords:	Atmospheric dynamics, Mars, 2300, 1007
DOI:	https://doi.org/10.3847/PSJ/ad06a9
Bibliographic Code:	2023PSJ.....4..222M
Abstract:	We use a spectral approach to analyze the pressure and wind data from the InSight mission and investigate the diurnal and seasonal trends. Our analyses show that the daytime pressure and wind spectra have slopes of approximately -1.7 and -1.3 and, therefore, do not follow the Kolmogorov scaling (as was also previously reported for a reduced data set in Banfield et al.). We find that the nighttime pressure spectral slope is close to -1 (as reported in Temel et al.), and that the wind speed spectral slope is close to -0.5, flatter than the theoretical slope expected for the shear-dominated regime. We observe strong nocturnal (likely shear-generated) turbulent behavior starting around L <SUB>s</SUB> = 150° (InSight sol 440) that shifts to progressively earlier local times before reaching the "5th season" (InSight sols 530-710) identified by Chatain et al.. The diurnal spectral slope analyses indicate an asymmetry in the diurnal behavior of the Martian boundary layer, with a slow growth and fast collapse mechanism. Finally, the low-frequency (5-30 mHz) pressure data exhibit large spectral slope oscillations. These occur particularly during the periods with a highly stable atmosphere and, therefore, may be linked to gravity wave activity.

Title:	Simulated Atmospheric Response to Large-Scale Dust Forcing and Implications for Martian Dust Storm Growth
Authors:	Wang, Huiqun; Toigo, Anthony D.; Richardson, Mark I.
Affiliation:	AA(Center for Astrophysics\|Harvard-Smithsonian, Cambridge, MA USA), AB(John Hopkins University Applied Physics Laboratory, Laurel, MD USA), AC(Aeolis Research, Chandler, AZ USA)
Journal:	Journal of Geophysical Research: Planets, Volume 128, Issue 10, article id. e2023JE007956.
Publication Date:	Oct 2023
Origin:	American Geophysical Union (AGU)
Keywords:	Mars, atmosphere, dust storm, model, circulation
Abstract Copyright:	2023. American Geophysical Union. All Rights Reserved.
DOI:	https://doi.org/10.1029/2023JE007956
Bibliographic Code:	2023JGRE..12807956W
Abstract:	The response of tidal, "weather," and intra-seasonal transient eddies in a global numerical model to dust imposed in different latitudinal bands and seasons has been examined in order to investigate the impact of regional scale dust storm episodes on large-scale circulation and hence on further dust storm development. The eddy kinetic energy and surface friction speed for each eddy group were derived using wavelet analysis from multi-year simulations and statistical comparisons were made among the experiments. Results show that different eddy categories respond differently to dust storm forcing, and that the responses are dependent upon both modeled storm location and season. These responses can be cast in terms of potential positive and negative feedbacks on large-scale dust storm development and have implications for the cascade of dust storms through different scales and circulation components. The model results suggest positive feedback between northern high latitude dust forcing and weather transients in the same latitudes in Quartober (L<SUB>s</SUB> = 185°-245°), which weakens or disappears in Sixtober (L<SUB>s</SUB> = 295°-360°). The results also suggest positive feedback between dust heating in the tropics/subtropics and tidal eddies, which may enhance the southward transport of "flushing" storms. However, southern high latitude dust forcing suppresses northern weather transients in both pseudo-season sextons, suggesting negative feedback which may terminate northern frontal/flushing dust storm sequences and hence weaken further development of a dust storm episode through this mechanism.

Title:	Dust Lifting Observations With the Mars Science Laboratory Navigation Cameras
Authors:	Guzewich, Scott D.; Mason, Emily L.; Lemmon, Mark T.; Newman, Claire E.; Lewis, Kevin W.
Affiliation:	AA(NASA Goddard Space Flight Center, Greenbelt, MD USA), AB(NASA Goddard Space Flight Center, Greenbelt, MD USA; University of Maryland Baltimore County, Catonsville, MD USA; Center for Research and Exploration in Space Science and Technology II, NASA, GSFC, Greenbelt, MD USA), AC(Space Science Institute, Boulder, CO USA), AD(Aeolis Research, Pasadena, CA USA), AE(Johns Hopkins University, Baltimore, MD USA)
Journal:	Journal of Geophysical Research: Planets, Volume 128, Issue 10, article id. e2023JE007959.
Publication Date:	Oct 2023
Origin:	American Geophysical Union (AGU)
Keywords:	Mars, dust, Mars Science Laboratory, dust devil, aeolian
Abstract Copyright:	2023. American Geophysical Union. All Rights Reserved.
DOI:	https://doi.org/10.1029/2023JE007959
Bibliographic Code:	2023JGRE..12807959G
Abstract:	Martian dust lifting is believed to occur through two primary mechanisms: dust devils and wind stress forced dust lifting. Gale Crater's varied terrain and meteorology provide a unique in situ perspective on Martian dust lifting, with the Mars Science Laboratory Curiosity rover passing through both conditions and locations detrimental to dust lifting (e.g., the crater floor) and those with active sand motion and frequent dust lifting (e.g., the Bagnold Dunes). Between L<SUB>s</SUB> = 248° in Mars Year 33 and L<SUB>s</SUB> = 51° in Mars Year 37, over ∼3.5 Mars years and 2,300 sols, the rover's Navigation Cameras took 1,260 dedicated image sequences to search for dust lifting. Approximately 42.7% of all sequences, and 9.5% of the total images have shown active dust lifting, both dust devils and linear/straight-line wind stress dust lifting. 79% of dust lifting events are classified as dust devils, while ∼16% are linear wind stress dust lifting and the remainder are of an indeterminate type. We analyze this large catalog of dust lifting events to provide ground truth on theoretical and model expectations of dust lifting and show that dust lifting in Gale Crater occurs throughout the Martian year, is strongly peaked in frequency near solar noon (even after accounting for observational biases), and that dust lifting shows an affinity for sand-covered surfaces which highlights the importance of saltating sand grains for Martian dust lifting in both dust devils and wind stress forced lifting.

Title:	Spatial extent of dust storm boundaries in the Mars Dust Activity Database
Authors:	Battalio, J. Michael; Wang, Huiqun; Richardson, Mark I.; Toigo, Anthony D.; Saidel, Morgan
Affiliation:	AA(Department of Earth and Planetary Sciences, Yale University, New Haven, CT, USA), AB(Smithsonian Astrophysical Observatory, Center for Astrophysics - Harvard & Smithsonian, Cambridge, MA, USA), AC(Aeolis Research, Chandler, AZ, USA), AD(Johns Hopkins University Applied Physics Laboratory, Laurel, MD, USA), AE(Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA, USA)
Journal:	Icarus, Volume 400, article id. 115567.
Publication Date:	Aug 2023
Origin:	Elsevier BV
Keywords:	Mars, Mars, atmosphere, Meteorology
Abstract Copyright:	(c) 2023 Elsevier Inc.
DOI:	https://doi.org/10.1016/j.icarus.2023.115567
Bibliographic Code:	2023Icar..40015567B
Abstract:	The Mars Dust Activity Database (MDAD) v1.1 is expanded to include all dust storm instance boundaries in MDAD v1.0 from the Mars Color Imager years (Mars Years 28-32). Dust storm boundaries are provided in two formats to ease adoption by the community: as netCDF masks and in comma separated value files. We demonstrate the utility of dust storm boundaries by showing how the frequency of dust storms evolves with season across the surface. The highest dust storm frequencies occur in the southern hemisphere around L<SUB>s</SUB> = 0° and L<SUB>s</SUB> = 270° and in the northern hemisphere around L<SUB>s</SUB> = 180° and L<SUB>s</SUB> = 300°.

Title:	Measurements of sound propagation in Mars' lower atmosphere
Authors:	Chide, Baptiste; Jacob, Xavier; Petculescu, Andi; Lorenz, Ralph D.; Maurice, Sylvestre; Seel, Fabian; Schröder, Susanne; Wiens, Roger C.; Gillier, Martin; Murdoch, Naomi; Lanza, Nina L.; Bertrand, Tanguy; Leighton, Timothy G.; Joseph, Phillip; Pilleri, Paolo; Mimoun, David; Stott, Alexander; de la Torre Juarez, Manuel; Hueso, Ricardo; Munguira, Asier; Sánchez-Lavega, Agustin; Martinez, German; Larmat, Carène; Lasue, Jérémie; Newman, Claire; Pla-Garcia, Jorge; Bernardi, Pernelle; Harri, Ari-Matti; Genzer, Maria; Lepinette, Alain
Affiliation:	AA(Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA), AB(Institut de Mécanique des Fluides de Toulouse, Université de Toulouse III Paul Sabatier, INP, CNRS, Toulouse, France), AC(Department of Physics, University of Louisiana at Lafayette, Lafayette, LA, USA), AD(Space Exploration Sector, Johns Hopkins Applied Physics Laboratory, Laurel, MD, USA), AE(Institut de Recherches en Astrophysique et Planétologie (IRAP), Toulouse, France), AF(Institute of Optical Sensor Systems, German Aerospace Center (DLR), Berlin, Germany), AG(Institute of Optical Sensor Systems, German Aerospace Center (DLR), Berlin, Germany), AH(Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN, USA), AI(Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France), AJ(Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France), AK(Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA), AL(LESIA, Observatoire de Paris, Université PSL, Sorbonne Université, Université de Paris, CNRS, Meudon, France), AM(Institute of Sound and Vibration Research, University of Southampton, Southampton, United Kingdom), AN(Institute of Sound and Vibration Research, University of Southampton, Southampton, United Kingdom), AO(Institut de Recherches en Astrophysique et Planétologie (IRAP), Toulouse, France), AP(Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France), AQ(Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France), AR(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA), AS(Física Aplicada, Escuela de Ingeniería de Bilbao, UPV/EHU, Bilbao, Spain), AT(Física Aplicada, Escuela de Ingeniería de Bilbao, UPV/EHU, Bilbao, Spain), AU(Física Aplicada, Escuela de Ingeniería de Bilbao, UPV/EHU, Bilbao, Spain), AV(Lunar and Planetary Institute, Universities Space Research Association, Houston, TX, USA), AW(Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA), AX(Institut de Recherches en Astrophysique et Planétologie (IRAP), Toulouse, France), AY(Aeolis Research, Chandler, AZ, USA), AZ(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), BA(LESIA, Observatoire de Paris, Université PSL, Sorbonne Université, Université de Paris, CNRS, Meudon, France), BB(Finnish Meteorological Institute, Helsinki, Finland), BC(Finnish Meteorological Institute, Helsinki, Finland), BD(Centro de Astrobiología (INTA-CSIC), Madrid, Spain)
Journal:	Earth and Planetary Science Letters, Volume 615, article id. 118200.
Publication Date:	Aug 2023
Origin:	Elsevier BV
Keywords:	Mars, acoustics, sound propagation, Mars 2020, Perseverance rover, SuperCam microphone, atmosphere, turbulence
Abstract Copyright:	(c) 2023 Elsevier Science B.V. All rights reserved.
DOI:	https://doi.org/10.1016/j.epsl.2023.118200
Bibliographic Code:	2023E&PSL.61518200C
Abstract:	Acoustics has become extraterrestrial and Mars provides a new natural laboratory for testing sound propagation models compared to those ones on Earth. Owing to the unique combination of a microphone and two sound sources, the Ingenuity helicopter and the SuperCam laser-induced sparks, the Mars 2020 Perseverance rover payload enables the in situ characterization of unique sound propagation properties of the low-pressure CO<SUB>2</SUB>-dominated Mars atmosphere. In this study, we show that atmospheric turbulence is responsible for a large variability in the sound amplitudes from laser-induced sparks. This variability follows the diurnal pattern of turbulence. In addition, acoustic measurements acquired over one Martian year reveal a variation of the sound intensity by a factor of 1.8 from a constant source due to the seasonal cycle of pressure and temperature that significantly modifies the acoustic impedance and shock-wave formation. Finally, we show that the evolution of the Ingenuity tones and laser spark amplitudes with distance is consistent with one of the existing sound absorption models, which is a key parameter for numerical simulations applied to geophysical experiments on CO<SUB>2</SUB>-rich atmospheres. Overall, these results demonstrate the potential of sound propagation to interrogate the Mars environment and will therefore help in the design of future acoustic-based experiments for Mars or other planetary atmospheres such as Venus and Titan.

Title:	Nocturnal Turbulence at Jezero Crater as Determined From MEDA Measurements and Modeling
Authors:	Pla-García, Jorge; Munguira, A.; Rafkin, S.; Newman, C.; Bertrand, T.; Martínez, G.; Hueso, R.; Sánchez-Lavega, A.; del Río Gaztelurrutia, T.; Stott, A.; Murdoch, N.; de la Torre Juárez, M.; Lemmon, M.; Chide, B.; Viúdez-Moreiras, D.; Savijarvi, H.; Richardson, M.; Marín, M.; Sebastian, E.; Lepinette-Malvitte, A.; Mora, L.; Rodríguez-Manfredi, J. A.
Affiliation:	AA(Centro de Astrobiología (CAB), CSIC-INTA, Madrid, Spain), AB(Universidad del País Vasco (UPV/EHU), Bilbao, Spain), AC(Southwest Research Institute, Boulder, CO USA), AD(Aeolis Research, Chandler, AZ USA), AE(LESIA, Observatoire de Paris, Paris, France), AF(Lunar and Planetary Institute, Houston, TX USA), AG(Universidad del País Vasco (UPV/EHU), Bilbao, Spain), AH(Universidad del País Vasco (UPV/EHU), Bilbao, Spain), AI(Universidad del País Vasco (UPV/EHU), Bilbao, Spain), AJ(Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France), AK(Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France), AL(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AM(Space Science Institute, Boulder, CO USA), AN(Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM USA), AO(Centro de Astrobiología (CAB), CSIC-INTA, Madrid, Spain), AP(Finnish Meteorological Institute, Helsinki, Finland), AQ(Aeolis Research, Chandler, AZ USA), AR(Centro de Astrobiología (CAB), CSIC-INTA, Madrid, Spain), AS(Centro de Astrobiología (CAB), CSIC-INTA, Madrid, Spain), AT(Centro de Astrobiología (CAB), CSIC-INTA, Madrid, Spain), AU(Centro de Astrobiología (CAB), CSIC-INTA, Madrid, Spain), AV(Centro de Astrobiología (CAB), CSIC-INTA, Madrid, Spain)
Journal:	Journal of Geophysical Research: Planets, Volume 128, Issue 8, article id. e2022JE007607.
Publication Date:	Aug 2023
Origin:	American Geophysical Union (AGU)
Abstract Copyright:	2023. The Authors.
DOI:	https://doi.org/10.1029/2022JE007607
Bibliographic Code:	2023JGRE..12807607P
Abstract:	Mars 2020 Mars Environmental Dynamics Analyzer (MEDA) instrument data acquired during half of a Martian year (L<SUB>s</SUB> 13°-180°), and modeling efforts with the Mars Regional Atmospheric Modeling System (MRAMS) and the Mars Climate Database (MCD) enable the study of the seasonal evolution and variability of nocturnal atmospheric turbulence at Jezero crater. Nighttime conditions in Mars's Planetary Boundary Layer are highly stable because of strong radiative cooling that efficiently inhibits convection. However, MEDA nighttime observations of simultaneous rapid fluctuations in horizontal wind speed and air temperatures suggest the development of nighttime turbulence in Jezero crater. Mesoscale modeling with MRAMS also shows a similar pattern and enables us to investigate the origins of this turbulence and the mechanisms at play. As opposed to Gale crater, less evidence of turbulence from breaking mountain wave activity was found in Jezero during the period studied with MRAMS. On the contrary, the model suggests that nighttime turbulence at Jezero crater is explained by increasingly strong wind shear produced by the development of an atmospheric bore-like disturbance at the nocturnal inversion interface. These atmospheric bores are produced by downslope winds from the west rim undercutting a strong low-level jet aloft from ∼19:00 to 01:00 LTST and from ∼01:00 LTST to dawn when undercutting weak winds aloft. The enhanced wind shear leads to a reduction in the Richardson number and an onset of mechanical turbulence. Once the critical Richardson Number is reached (Ri ∼ <0.25), shear instabilities can mix warmer air aloft down to the surface.

Title:	Twilight Mesospheric Clouds in Jezero as Observed by MEDA Radiation and Dust Sensor (RDS)
Authors:	Toledo, D.; Gómez, L.; Apéstigue, V.; Arruego, I.; Smith, M.; Munguira, A.; Martínez, G.; Patel, P.; Sanchez-Lavega, A.; Lemmon, M.; Tamppari, L.; Viudez-Moreiras, D.; Hueso, R.; Vicente-Retortillo, A.; Newman, C.; Lorenz, R.; Yela, M.; Juarez, M. de la Torre; Rodriguez-Manfredi, J. A.
Affiliation:	AA(Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain), AB(Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain), AC(Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain), AD(Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain), AE(NASA Godard Space Flight Center, Greenbelt, MD USA), AF(Universidad del País Vasco UPV/EHU, Bilbao, Spain), AG(Lunar and Planetary Institute, Universities Space Research Association, Houston, TX USA), AH(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AI(Universidad del País Vasco UPV/EHU, Bilbao, Spain), AJ(Space Science Institute, Boulder, CO USA), AK(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AL(Centro de Atrobiología (INTA-CSIC), Torrejón de Ardoz, Madrid, Spain), AM(Universidad del País Vasco UPV/EHU, Bilbao, Spain), AN(Centro de Atrobiología (INTA-CSIC), Torrejón de Ardoz, Madrid, Spain), AO(Aeolis Research, Chandler, AZ USA), AP(Johns Hopkins Applied Physics Laboratory, Laurel, MD USA), AQ(Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain), AR(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AS(Centro de Atrobiología (INTA-CSIC), Torrejón de Ardoz, Madrid, Spain)
Journal:	Journal of Geophysical Research: Planets, Volume 128, Issue 7, article id. e2023JE007785.
Publication Date:	Jul 2023
Origin:	American Geophysical Union (AGU)
Abstract Copyright:	2023 The Authors.
DOI:	https://doi.org/10.1029/2023JE007785
Bibliographic Code:	2023JGRE..12807785T
Abstract:	The Mars Environmental Dynamics Analyzer instrument, on board NASA's Mars 2020 Perseverance rover, includes a number of sensors to characterize the Martian atmosphere. One of these sensors is the Radiation and Dust Sensor (RDS) that measures the solar irradiance at different wavelengths and geometries. We analyzed the RDS observations made during twilight for the period between sol 71 and 492 of the mission (Ls 39°-262°, Mars Year 36) to characterize the clouds over the Perseverance rover site. Using the ratio between the irradiance at zenith at 450 and 750 nm, we inferred that the main constituent of the detected high-altitude aerosol layers was ice from Ls = 39°-150° (cloudy period), and dust from Ls 150°-262°. A total of 161 twilights were analyzed in the cloudy period using a radiative transfer code and we found: (a) signatures of clouds/hazes in the signals in 58% of the twilights; (b) most of the clouds had altitudes between 40 and 50 km, suggesting water ice composition, and had particle sizes between 0.6 and 2 µm; (c) the cloud activity at sunrise is slightly higher that at sunset, likely due to the differences in temperature; (d) the time period with more cloud detections and with the greatest cloud opacities is during Ls 120°-150°; and (e) a notable decrease in the cloud activity around aphelion, along with lower cloud altitudes and opacities. This decrease in cloud activity indicates lower concentrations of water vapor or cloud condensation nuclei (dust) around this period in the Martian mesosphere.

Title:	Samples Collected From the Floor of Jezero Crater With the Mars 2020 Perseverance Rover
Authors:	Simon, J. I.; Hickman-Lewis, K.; Cohen, B. A.; Mayhew, L. E.; Shuster, D. L.; Debaille, V.; Hausrath, E. M.; Weiss, B. P.; Bosak, T.; Zorzano, M.-P.; Amundsen, H. E. F.; Beegle, L. W.; Bell, J. F.; Benison, K. C.; Berger, E. L.; Beyssac, O.; Brown, A. J.; Calef, F.; Casademont, T. M.; Clark, B.; Clavé, E.; Crumpler, L.; Czaja, A. D.; Fairén, A. G.; Farley, K. A.; Flannery, D. T.; Fornaro, T.; Forni, O.; Gómez, F.; Goreva, Y.; Gorin, A.; Hand, K. P.; Hamran, S.-E.; Henneke, J.; Herd, C. D. K.; Horgan, B. H. N.; Johnson, J. R.; Joseph, J.; Kronyak, R. E.; Madariaga, J. M.; Maki, J. N.; Mandon, L.; McCubbin, F. M.; McLennan, S. M.; Moeller, R. C.; Newman, C. E.; Núñez, J. I.; Pascuzzo, A. C.; Pedersen, D. A.; Poggiali, G.; Pinet, P.; Quantin-Nataf, C.; Rice, M.; Rice, J. W.; Royer, C.; Schmidt, M.; Sephton, M.; Sharma, S.; Siljeström, S.; Stack, K. M.; Steele, A.; Sun, V. Z.; Udry, A.; VanBommel, S.; Wadhwa, M.; Wiens, R. C.; Williams, A. J.; Williford, K. H.
Affiliation:	AA(Center for Isotope Cosmochemistry and Geochronology, Astromaterials Research and Exploration Science, NASA Johnson Space Center, Houston, TX USA), AB(The Natural History Museum, London, UK; Dipartimento BiGeA, Università di Bologna, Bologna, Italy), AC(NASA Goddard Space Flight Center, Greenbelt, MD USA), AD(Department of Geological Sciences, University of Colorado Boulder, Boulder, CO USA), AE(University of California, Berkeley, Berkeley, CA USA), AF(Universitélibre de Bruxelles, Brussels, Belgium), AG(Department of Geosciences, University of Nevada, Las Vegas, Las Vegas, NV USA), AH(Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA USA), AI(Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA USA), AJ(Centro de Astrobiologia (CAB), CSIC-INTA, Madrid, Spain), AK(University of Oslo, Norwegian Research Council, Oslo, Norway), AL(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AM(Arizona State University, Tempe, AZ USA), AN(West Virginia University, Morgantown, WV USA), AO(Texas State University, Jacobs JETS, NASA Johnsons Space Center, Houston, TX USA), AP(Institut de Minéralogie, Physique des Matériaux et Cosmochimie, CNRS UMR 7590, Sorbonne Université, Muséum National d'Histoire Naturelle, Paris, France), AQ(Plancius Research, Severna Park, MD USA), AR(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AS(University of Oslo, Norwegian Research Council, Oslo, Norway), AT(Space Science Institute, Boulder, CO USA), AU(CELIA, Université de Bordeaux, CNRS, CEA, Bordeaux, France), AV(New Mexico Museum of Natural History and Science, Albuquerque, NM USA), AW(Department of Geology, University of Cincinnati, Cincinnati, OH USA), AX(Centro de Astrobiologia (CAB), CSIC-INTA, Madrid, Spain; Department Astronomy, Cornell University, Ithaca, NY USA), AY(California Institute of Technology, Pasadena, CA USA), AZ(Queensland University of Technology, Brisbane, QL Australia), BA(INAF-Astrophysical Observatory of Arcetri, Florence, Italy), BB(Institut de Recherche en Astrophysique et Planétologie (IRAP), Université de Toulouse, CNRS, UPS, CNES, Toulouse, France), BC(Centro de Astrobiologia (CAB), CSIC-INTA, Madrid, Spain), BD(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), BE(Universitélibre de Bruxelles, Brussels, Belgium), BF(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), BG(University of Oslo, Norwegian Research Council, Oslo, Norway), BH(Danmarks Tekniske Universitet, National Space Institute, Lyngby, Denmark), BI(Department of Earth and Atmospheric Sciences, University of Alberta, Edmonton, AB Canada), BJ(Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN USA), BK(Johns Hopkins University Applied Physics Laboratory, Laurel, MD USA), BL(Cornell University, Ithaca, NY USA), BM(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), BN(Department of Analytical Chemistry, University of the Basque Country (UPV/EHU), Leioa, Spain), BO(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), BP(LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université de Paris, Meudon, France), BQ(Astromaterials Research and Exploration Science, NASA Johnson Space Center, Houston, TX USA), BR(Department of Geosciences, Stony Brook University, Stony Brook, NY USA), BS(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), BT(Aeolis Research, Chandler, AZ USA), BU(Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN USA), BV(Malin Space Science Systems, San Diego, CA USA), BW(Department of Earth and Atmospheric Sciences, University of Alberta, Edmonton, AB Canada), BX(INAF-Astrophysical Observatory of Arcetri, Firenze, Italy), BY(Institut de Recherche en Astrophysique et Planétologie (IRAP), Université de Toulouse, CNRS, UPS, CNES, Toulouse, France), BZ(Laboratoire de Géologie de Lyon, Université Lyon, Bâtiment Géode, Villeurbanne, France), CA(Western Washington University, Bellingham, WA USA), CB(Arizona State University, Tempe, AZ USA), CC(CELIA, Université de Bordeaux, CNRS, CEA, Bordeaux, France), CD(Department of Earth Sciences, Brock University, St. Catharines, ON Canada), CE(Department of Earth Science and Engineering, Imperial College London, London, UK), CF(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), CG(RISE Research Institutes of Sweden, Stockholm, Sweden), CH(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), CI(Earth and Planetary Laboratory, Carnegie Institution for Science, Washington, DC USA), CJ(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), CK(Department of Geosciences, University of Nevada, Las Vegas, Las Vegas, NV USA), CL(McDonnell Center for the Space Sciences, Department of Earth and Planetary Sciences, Washington University in St. Louis, St. Louis, MO USA), CM(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA; Arizona State University, Tempe, AZ USA), CN(Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN USA), CO(Department of Geological Sciences, University of Florida, Gainesville, FL USA), CP(Blue Marble Space Institute of Science, Seattle, WA USA)
Journal:	Journal of Geophysical Research: Planets, Volume 128, Issue 6, article id. e2022JE007474.
Publication Date:	Jun 2023
Origin:	American Geophysical Union (AGU)
Keywords:	Mars 2020, Mars sample return, rock core, Jezero Crater
Abstract Copyright:	2023. American Geophysical Union. All Rights Reserved.
DOI:	https://doi.org/10.1029/2022JE007474
Bibliographic Code:	2023JGRE..12807474S
Abstract:	The first samples collected by the Mars 2020 mission represent units exposed on the Jezero Crater floor, from the potentially oldest Séítah formation outcrops to the potentially youngest rocks of the heavily cratered Máaz formation. Surface investigations reveal landscape-to-microscopic textural, mineralogical, and geochemical evidence for igneous lithologies, some possibly emplaced as lava flows. The samples contain major rock-forming minerals such as pyroxene, olivine, and feldspar, accessory minerals including oxides and phosphates, and evidence for various degrees of aqueous activity in the form of water-soluble salt, carbonate, sulfate, iron oxide, and iron silicate minerals. Following sample return, the compositions and ages of these variably altered igneous rocks are expected to reveal the geophysical and geochemical nature of the planet's interior at the time of emplacement, characterize martian magmatism, and place timing constraints on geologic processes, both in Jezero Crater and more widely on Mars. Petrographic observations and geochemical analyses, coupled with geochronology of secondary minerals, can also reveal the timing of aqueous activity as well as constrain the chemical and physical conditions of the environments in which these minerals precipitated, and the nature and composition of organic compounds preserved in association with these phases. Returned samples from these units will help constrain the crater chronology of Mars and the global evolution of the planet's interior, for understanding the processes that formed Jezero Crater floor units, and for constraining the style and duration of aqueous activity in Jezero Crater, past habitability, and cycling of organic elements in Jezero Crater.

Title:	Overview and Results From the Mars 2020 Perseverance Rover's First Science Campaign on the Jezero Crater Floor
Authors:	Sun, Vivian Z.; Hand, Kevin P.; Stack, Kathryn M.; Farley, Ken A.; Simon, Justin I.; Newman, Claire; Sharma, Sunanda; Liu, Yang; Wiens, Roger C.; Williams, Amy J.; Tosca, Nicholas; Alwmark, Sanna; Beyssac, Olivier; Brown, Adrian; Calef, Fred; Cardarelli, Emily L.; Clavé, Elise; Cohen, Barbara; Corpolongo, Andrea; Czaja, Andrew D.; Del Sesto, Tyler; Fairen, Alberto; Fornaro, Teresa; Fouchet, Thierry; Garczynski, Brad; Gupta, Sanjeev; Herd, Chris D. K.; Hickman-Lewis, Keyron; Horgan, Briony; Johnson, Jeffrey; Kinch, Kjartan; Kizovski, Tanya; Kronyak, Rachel; Lange, Robert; Mandon, Lucia; Milkovich, Sarah; Moeller, Robert; Núñez, Jorge; Paar, Gerhard; Pyrzak, Guy; Quantin-Nataf, Cathy; Shuster, David L.; Siljestrom, Sandra; Steele, Andrew; Tice, Michael; Toupet, Olivier; Udry, Arya; Vaughan, Alicia; Wogsland, Brittan
Affiliation:	AA(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AB(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AC(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AD(California Institute of Technology, Pasadena, CA USA), AE(NASA Johnson Space Center, Houston, TX USA), AF(Aeolis Research, Chandler, AZ USA), AG(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AH(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AI(Purdue University, West Lafayette, IN USA), AJ(Department of Geological Sciences, University of Florida, Gainsville, FL USA), AK(University of Cambridge, Cambridge, UK), AL(Niels Bohr Institute, University of Copenhagen, Copenhagen, Denmark; Department of Geology, Lund University, Lund, Sweden), AM(CNRS, Muséum National d'Histoire Naturelle, Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, Sorbonne Université, Paris, France), AN(Plancius Research, Severna Park, MD USA), AO(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AP(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AQ(Centre Lasers Intenses et Applications, CNRS, CEA, Université de Bordeaux, Bordeaux, France), AR(NASA Goddard Spaceflight Center, Greenbelt, MD USA), AS(Department of Geology, University of Cincinnati, Cincinnati, OH USA), AT(Department of Geology, University of Cincinnati, Cincinnati, OH USA), AU(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AV(Centro de Astrobiologia (CSIC-INTA), Madrid, Spain; Department Astronomy, Cornell University, Ithaca, NY USA), AW(INAF-Astrophysical Observatory of Arcetri, Florence, Italy), AX(LESIA, Observatoire de Paris, CNRS, Université PSL, Sorbonne Université, Université Paris Cité, Meudon, France), AY(Purdue University, West Lafayette, IN USA), AZ(Imperial College London, London, UK), BA(University of Alberta, Edmonton, AB Canada), BB(Natural History Museum, London, UK; Dipartimento di Scienze Biologiche, Geologiche e Ambientali, Università di Bologna, Bologna, Italy), BC(Purdue University, West Lafayette, IN USA), BD(Johns Hopkins University Applied Physics Laboratory, Laurel, MD USA), BE(Niels Bohr Institute, University of Copenhagen, Copenhagen, Denmark), BF(Brock University, St. Catharines, ON Canada), BG(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), BH(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), BI(LESIA, Observatoire de Paris, CNRS, Université PSL, Sorbonne Université, Université Paris Cité, Meudon, France), BJ(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), BK(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), BL(Johns Hopkins University Applied Physics Laboratory, Laurel, MD USA), BM(Joanneum Research,, Graz, Austria), BN(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), BO(Laboratoire de Géologie de Lyon, Université Lyon, Villeurbanne, France), BP(University of California, Berkeley, Berkeley, CA USA), BQ(RISE Research Institutes of Sweden, Gothenburg, Sweden), BR(NASA Goddard Spaceflight Center, Greenbelt, MD USA; Carnegie Institute Washington, Washington, DC USA), BS(Department of Geology and Geophysics, Texas A&M University, College Station, TX USA), BT(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), BU(University of Nevada, Las Vegas, NV USA), BV(United States Geological Survey, Flagstaff, AZ USA), BW(University of Tennessee, Knoxville, TN USA)
Journal:	Journal of Geophysical Research: Planets, Volume 128, Issue 6, article id. e2022JE007613.
Publication Date:	Jun 2023
Origin:	American Geophysical Union (AGU)
Keywords:	Mars, Perseverance, rover, Jezero
Abstract Copyright:	2023 Jet Propulsion Laboratory, California Institute of Technology and The Authors. Government sponsorship acknowledged. This article has been contributed to by U.S. Government employees and their work is in the public domain in the USA.
DOI:	https://doi.org/10.1029/2022JE007613
Bibliographic Code:	2023JGRE..12807613S
Abstract:	The Mars 2020 Perseverance rover landed in Jezero crater on 18 February 2021. After a 100-sol period of commissioning and the Ingenuity Helicopter technology demonstration, Perseverance began its first science campaign to explore the enigmatic Jezero crater floor, whose igneous or sedimentary origins have been much debated in the scientific community. This paper describes the campaign plan developed to explore the crater floor's Máaz and Séítah formations and summarizes the results of the campaign between sols 100-379. By the end of the campaign, Perseverance had traversed more than 5 km, created seven abrasion patches, and sealed nine samples and a witness tube. Analysis of remote and proximity science observations show that the Máaz and Séítah formations are igneous in origin and composed of five and two geologic members, respectively. The Séítah formation represents the olivine-rich cumulate formed from differentiation of a slowly cooling melt or magma body, and the Máaz formation likely represents a separate series of lava flows emplaced after Séítah. The Máaz and Séítah rocks also preserve evidence of multiple episodes of aqueous alteration in secondary minerals like carbonate, Fe/Mg phyllosilicates, sulfates, and perchlorate, and surficial coatings. Post-emplacement processes tilted the rocks near the Máaz-Séítah contact and substantial erosion modified the crater floor rocks to their present-day expressions. Results from this crater floor campaign, including those obtained upon return of the collected samples, will help to build the geologic history of events that occurred in Jezero crater and provide time constraints on the formation of the Jezero delta.

Title:	Atmospheric CO<SUB>2</SUB> Depletion Near the Surface in the Martian Polar Regions
Authors:	Piqueux, Sylvain; Hayne, Paul O.; Kleinböhl, Armin; Kass, David M.; Schreier, Mathias; McCleese, Daniel J.; Richardson, Mark I.; Schofield, John T.; Heavens, Nicholas; Shirley, James H.
Affiliation:	AA(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AB(Department of Astrophysical and Planetary Sciences, Laboratory for Atmospheric and Space Physics, University of Colorado Boulder, Boulder, CO USA), AC(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AD(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AE(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AF(Synoptic Sciences, Pasadena, CA USA), AG(Aeolis Research, Chandler, AZ USA), AH(Synoptic Sciences, Pasadena, CA USA), AI(Space Science Institute, Boulder, CO USA), AJ(TorqueFX, Simi Valley, CA USA)
Journal:	Journal of Geophysical Research: Planets, Volume 128, Issue 6, article id. e2022JE007332.
Publication Date:	Jun 2023
Origin:	American Geophysical Union (AGU)
Keywords:	Mars, ice, depletion, temperature, CO<SUB>2</SUB>
Abstract Copyright:	2023 American Geophysical Union. All Rights Reserved. California Institute of Technology. Government sponsorship acknowledged.
DOI:	https://doi.org/10.1029/2022JE007332
Bibliographic Code:	2023JGRE..12807332P
Abstract:	The kinetic temperature of the Martian seasonal caps is controlled by the partial pressure of atmospheric CO<SUB>2</SUB> at the surface. When carbon dioxide condenses, typically near the poles, light non-condensable species (Ar, N<SUB>2</SUB>, CO, etc.) accumulate in the atmosphere, resulting in a decrease of the CO<SUB>2</SUB> partial pressure and depressing the local frost point temperature. The buoyant air should mix laterally and vertically within the polar vortices. Observations show that the Martian seasonal caps' kinetic temperatures are ∼0-4 K below the expected CO<SUB>2</SUB> frost point, depending on latitude and season, indicating atmospheric CO<SUB>2</SUB> gas depletion at the surface/atmosphere interface. In the North and South, we find relatively similar non-condensable peak enhancement factors (e.g., EF<SUB>NC</SUB> ∼ 6-8, up to ∼8.7 in the North) at most latitudes, confirming the efficient meridional mixing within the polar vortices, despite steep surface condensation gradients. In the South, this surface enhancement is similar to column-integrated values derived from Gamma Ray Spectrometer data, indicating efficient vertical mixing. But in the North, the surface depletion is much larger than in the entire column, suggesting poor vertical mixing. Reduced infrared emission of the seasonal caps stemming from CO<SUB>2</SUB> depletion is not a major energy balance factor. This work illustrates how the atmosphere's composition at the surface can be significantly different from column-integrated values.

Title:	Wind and Turbulence Observations With the Mars Microphone on Perseverance
Authors:	Stott, Alexander E.; Murdoch, Naomi; Gillier, Martin; Banfield, Don; Bertrand, Tanguy; Chide, Baptiste; De la Torre Juarez, Manuel; Hueso, Ricardo; Lorenz, Ralph; Martinez, German; Munguira, Asier; Mora Sotomayor, Luis; Navarro, Sara; Newman, Claire; Pilleri, Paolo; Pla-Garcia, Jorge; Rodriguez-Manfredi, Jose Antonio; Sanchez-Lavega, Agustin; Smith, Michael; Viudez Moreiras, Daniel; Williams, Nathan; Maurice, Sylvestre; Wiens, Roger C.; Mimoun, David
Affiliation:	AA(Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France), AB(Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France), AC(Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France), AD(NASA Ames, Mountain View, CA USA), AE(Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique (LESIA), Observatoire de Paris-PSL, CNRS, Sorbonne Université, Université de Paris Cité, Meudon, France), AF(Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM USA), AG(Jet Propulsion Laboratory—California Institute of Technology, Pasadena, CA USA), AH(Fisica Aplicada, Escuela de Ingeniería de Bilbao, Universidad del País Vasco UPV/EHU, Bilbao, Spain), AI(Johns Hopkins Applied Physics Lab, Laurel, MD USA), AJ(Lunar and Planetary Institute, USRA, Houston, TX USA; University of Michigan, Ann Arbor, MI USA), AK(Fisica Aplicada, Escuela de Ingeniería de Bilbao, Universidad del País Vasco UPV/EHU, Bilbao, Spain), AL(Centro de Astrobiologia (CAB), CSIC-INTA, Madrid, Spain), AM(Centro de Astrobiologia (CAB), CSIC-INTA, Madrid, Spain), AN(Aeolis Research, Chandler, AZ USA), AO(CNRS, CNES, Institut de Recherche en Astrophysique et Planétologie (IRAP), Université de Toulouse 3 Paul Sabatier, Toulouse, France), AP(Centro de Astrobiologia (CAB), CSIC-INTA, Madrid, Spain), AQ(Centro de Astrobiologia (CAB), CSIC-INTA, Madrid, Spain), AR(Fisica Aplicada, Escuela de Ingeniería de Bilbao, Universidad del País Vasco UPV/EHU, Bilbao, Spain), AS(Goddard Space Flight Center, Greenbelt, MD USA), AT(Centro de Astrobiologia (CAB), CSIC-INTA, Madrid, Spain), AU(Jet Propulsion Laboratory—California Institute of Technology, Pasadena, CA USA), AV(CNRS, CNES, Institut de Recherche en Astrophysique et Planétologie (IRAP), Université de Toulouse 3 Paul Sabatier, Toulouse, France), AW(Purdue University, West Lafayette, IN USA), AX(Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France)
Journal:	Journal of Geophysical Research: Planets, Volume 128, Issue 5, article id. e2022JE007547.
Publication Date:	May 2023
Origin:	American Geophysical Union (AGU)
Keywords:	Mars, high frequency winds, planetary boundary layer, turbulence
Abstract Copyright:	2023. The Authors.
DOI:	https://doi.org/10.1029/2022JE007547
Bibliographic Code:	2023JGRE..12807547S
Abstract:	We utilize SuperCam's Mars microphone to provide information on wind speed and turbulence at high frequencies on Mars. To do so, we first demonstrate the sensitivity of the microphone signal level to wind speed, yielding a power law dependence. We then show the relationship between the microphone signal level and pressure, air and ground temperatures. A calibration function is constructed using Gaussian process regression (a machine learning technique) taking the microphone signal and air temperature as inputs to produce an estimate of the wind speed. This provides a high rate wind speed estimate on Mars, with a sample every 0.01 s. As a result, we determine the fast fluctuations of the wind at Jezero crater which highlights the nature of wind gusts over the Martian day. To analyze the turbulent behavior of this wind speed estimate, we calculate its normalized standard deviation, known as gustiness. To characterize the behavior of this high frequency turbulent intensity at Jezero crater, correlations are shown between the evaluated gustiness statistic and pressure drop rates/sizes, temperature and energy fluxes. This has implications for future atmospheric models on Mars, taking into account turbulence at the finest scales.

Title:	Unstructured grid dynamical modeling of planetary atmospheres using planetMPAS: The influence of the rigid lid, computational efficiency, and examples of Martian and Jovian application
Authors:	Lian, Yuan; Richardson, Mark I.
Affiliation:	AA(Aeolis Research, Chandler, AZ, 85224, USA), AB(Aeolis Research, Chandler, AZ, 85224, USA)
Journal:	Planetary and Space Science, Volume 229, article id. 105663.
Publication Date:	May 2023
Origin:	Elsevier BV
Keywords:	Astrophysics - Earth and Planetary Astrophysics
Abstract Copyright:	(c) 2023 The Authors
DOI:	https://doi.org/10.1016/j.pss.2023.105663
Bibliographic Code:	2023P&SS..22905663L
Abstract:	We present a new planetary global circulation model, planetMPAS, based on the state-of-the-art NCAR MPAS (Model for Prediction Across Scales) General Circulation Model. Taking advantage of the cross compatibility between WRF (Weather Research and Forecasting Model) and MPAS, planetMPAS includes most of the planetWRF physics parameterization schemes for terrestrial planets such as Mars and Titan. PlanetMPAS also includes a set of physics that represents radiative transfer, dry convection, moist convection and its associated microphysics for the Jovian atmosphere. We demonstrate that, despite the rigid-lid approximation, planetMPAS is suitable to simulate the climate systems in the Martian and Jovian atmospheres. Simulations using planetMPAS show that the new model can reproduce many aspects of the observed features on Mars and Jupiter, such as the seasonal CO2 cycle, polar argon enrichment, zonal mean temperature, and qualitative dust opacity on Mars, as well as the equatorial superrotation and banded zonal wind patterns on Jupiter.

Title:	Dust Lifting Through Surface Albedo Changes at Jezero Crater, Mars
Authors:	Vicente-Retortillo, A.; Martínez, G. M.; Lemmon, M. T.; Hueso, R.; Johnson, J. R.; Sullivan, R.; Newman, C. E.; Sebastián, E.; Toledo, D.; Apéstigue, V.; Arruego, I.; Munguira, A.; Sánchez-Lavega, A.; Murdoch, N.; Gillier, M.; Stott, A.; Mora-Sotomayor, L.; Bertrand, T.; Tamppari, L. K.; Juárez, M. de la Torre; Rodríguez-Manfredi, J.-A.
Affiliation:	AA(Centro de Astrobiología (INTA-CSIC), Madrid, Spain; University of Michigan, Ann Arbor, MI USA), AB(University of Michigan, Ann Arbor, MI USA; Lunar and Planetary Institute, USRA, Houston, TX USA), AC(Space Science Institute, Boulder, CO USA), AD(Física Aplicada, Escuela de Ingeniería, Universidad del País Vasco (UPV/EHU), Bilbao, Spain), AE(Johns Hopkins University Applied Physics Laboratory, Laurel, MD USA), AF(CCAPS, Cornell University, Ithaca, NY USA), AG(Aeolis Research, Chandler, AZ USA), AH(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AI(Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain), AJ(Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain), AK(Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain), AL(Física Aplicada, Escuela de Ingeniería, Universidad del País Vasco (UPV/EHU), Bilbao, Spain), AM(Física Aplicada, Escuela de Ingeniería, Universidad del País Vasco (UPV/EHU), Bilbao, Spain), AN(Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France), AO(Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France), AP(Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France), AQ(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AR(LESIA, Paris Observatory, Meudon, France), AS(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AT(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AU(Centro de Astrobiología (INTA-CSIC), Madrid, Spain)
Journal:	Journal of Geophysical Research: Planets, Volume 128, Issue 4, article id. e2022JE007672.
Publication Date:	Apr 2023
Origin:	American Geophysical Union (AGU)
Keywords:	albedo change, dust lifting, Mars 2020, dust devil, dust storm, MEDA
Abstract Copyright:	2023. The Authors.
DOI:	https://doi.org/10.1029/2022JE007672
Bibliographic Code:	2023JGRE..12807672V
Abstract:	We identify temporal variations in surface albedo at Jezero crater using first-of-their-kind high-cadence in-situ measurements of reflected shortwave radiation during the first 350 sols of the Mars 2020 mission. Simultaneous Mars Environmental Dynamics Analyzer (MEDA) measurements of pressure, radiative fluxes, winds, and sky brightness indicate that these albedo changes are caused by dust devils under typical conditions and by a dust storm at L<SUB>s</SUB> ∼ 155°. The 17% decrease in albedo caused by the dust storm is one order of magnitude larger than the most apparent changes caused during quiescent periods by dust devils. Spectral reflectance measurements from Mastcam-Z images before and after the storm indicate that the decrease in albedo is mainly caused by dust removal. The occurrence of albedo changes is affected by the intensity and proximity of the convective vortex, and the availability and mobility of small particles at the surface. The probability of observing an albedo change increases with the magnitude of the pressure drop (∆P): changes were detected in 3.5%, 43%, and 100% of the dust devils with ∆P < 2.5 Pa, ∆P > 2.5 Pa and ∆P > 4.5 Pa, respectively. Albedo changes were associated with peak wind speeds above 15 m·s<SUP>-1</SUP>. We discuss dust removal estimates, the observed surface temperature changes coincident with albedo changes, and implications for solar-powered missions. These results show synergies between multiple instruments (MEDA, Mastcam-Z, Navcam, and the Supercam microphone) that improve our understanding of aeolian processes on Mars.

Title:	Results from InSight Robotic Arm Activities
Authors:	Golombek, M.; Hudson, T.; Bailey, P.; Balabanska, N.; Marteau, E.; Charalambous, C.; Baker, M.; Lemmon, M.; White, B.; Lorenz, R. D.; Spohn, T.; Maki, J.; Kallemeyn, P.; Garvin, J. B.; Newman, C.; Hurst, K.; Murdoch, N.; Williams, N.; Banerdt, W. B.; Lognonné, P.; Delage, P.; Lapeyre, R.; Gaudin, E.; Yana, C.; Verdier, N.; Panning, M.; Trebi-Ollennu, A.; Ali, K.; Mittelholz, A.; Johnson, C.; Langlais, B.; Warner, N.; Grant, J.; Daubar, I. J.; Ansan, V.; Vrettos, C.; Spiga, A.; Banfield, D.; Gomez, A.; Mishra, P.; Dotson, R.; Krause, C.; Sainton, G.; Gabsi, T.
Affiliation:	AA(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA), AB(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA), AC(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA), AD(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA), AE(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA), AF(Imperial College, London, UK), AG(National Air and Space Museum, Smithsonian Institution, CEPS, Washington, DC, USA), AH(Space Science Institute, Boulder, CO, USA), AI(Lockheed Martin Space Systems Company, Littleton, CO, USA), AJ(Johns Hopkins Applied Physics Laboratory, Laurel, MD, USA), AK(International Space Science Institute, Bern, Switzerland; German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany; German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany), AL(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA), AM(Lockheed Martin Space Systems Company, Littleton, CO, USA), AN(NASA Goddard Space Flight Center, 8800 Greenbelt Road, Greenbelt, MD, USA), AO(Aeolis Research, Chandler, AZ, USA), AP(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA), AQ(Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France), AR(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA), AS(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA), AT(Institut de Physique du Globe de Paris-Sorbonne Paris Cité, Université Paris Cité, Paris, France), AU(Ecole des Ponts Paris Tech, Laboratoire Navier/CERMES, CNRS, Marne la Vallée, France), AV(Centre National d'Études Spatiales, Toulouse, France), AW(Centre National d'Études Spatiales, Toulouse, France), AX(Centre National d'Études Spatiales, Toulouse, France), AY(Centre National d'Études Spatiales, Toulouse, France), AZ(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA), BA(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA), BB(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA), BC(Department of Earth and Planetary Sciences, Harvard University, Cambridge, MA, USA), BD(Department of Earth, Ocean and Atmospheric Sciences, The University of British Columbia, Vancouver, Canada; Planetary Science Institute, Tucson, AZ, USA; Planetary Science Institute, Tucson, AZ, USA), BE(CNRS, UMR 6112, Laboratoire de Planétologie et Géosciences, Nantes Université, Nantes, France), BF(Department of Geological Sciences, SUNY Geneseo, 1 College Circle, Geneseo, NY, USA), BG(National Air and Space Museum, Smithsonian Institution, CEPS, Washington, DC, USA), BH(Earth, Environmental, and Planetary Sciences, Brown University, Providence, RI, USA), BI(CNRS, UMR 6112, Laboratoire de Planétologie et Géosciences, Nantes Université, Nantes, France), BJ(Technical University of Kaiserslautern, Kaiserslautern, Germany), BK(Laboratoire de Météorologie Dynamique/Institut Pierre-Simon Laplace (LMD/IPSL), Centre National de la Recherche Scientifique (CNRS), Sorbonne Université, Paris, France), BL(NASA Ames Research Center, Moffett Field, CA, USA), BM(California Institute of Technology, Pasadena, CA, USA), BN(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA), BO(Quantaero, 1 E. Liberty St., Ste 600, Reno, NV, USA), BP(German Aerospace Center (DLR), Microgravity User Support Center (MUSC), Cologne, Germany), BQ(Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France), BR(Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France)
Journal:	Space Science Reviews, Volume 219, Issue 3, article id.20.
Publication Date:	Apr 2023
Origin:	Springer Science and Business Media LLC
Keywords:	Mars, Arm activities, InSight mission, Soil mechanics, Geology, Eolian activity
DOI:	https://doi.org/10.1007/s11214-023-00964-0
Bibliographic Code:	2023SSRv..219...20G
Abstract:	The InSight lander carried an Instrument Deployment System (IDS) that included an Instrument Deployment Arm (IDA), scoop, five finger "claw" grapple, forearm-mounted Instrument Deployment Camera (IDC) requiring arm motion to image a target, and lander-mounted Instrument Context Camera (ICC), designed to image the workspace, and to place the instruments onto the surface. As originally proposed, the IDS included a previously built arm and flight spare black and white cameras and had no science objectives or requirements, or expectation to be used after instrument deployment (90 sols). During project development the detectors were upgraded to color, and it was recognized that the arm could be used to carry out a wide variety of activities that would enable both geology and physical properties investigations. During surface operations for two martian years, the IDA was used during major campaigns to image the surface around the lander, to deploy the instruments, to assist the mole in penetrating beneath the surface, to bury a portion of the seismometer tether, to clean dust from the solar arrays to increase power, and to conduct a surface geology investigation including soil mechanics and physical properties experiments. No other surface mission has engaged in such a sustained and varied campaign of arm and scoop activities directed at such a diverse suite of objectives. Images close to the surface and continuous meteorology measurements provided important constraints on the threshold friction wind speed needed to initiate aeolian saltation and surface creep. The IDA was used extensively for almost 22 months to assist the mole in penetrating into the subsurface. Soil was scraped into piles and dumped onto the seismometer tether six times in an attempt to bury the tether and ∼30 % was entrained in the wind and dispersed downwind 1-2 m, darkening the surface. Seven solar array cleaning experiments were conducted by dumping scoops of soil from 35 cm above the lander deck during periods of high wind that dispersed the sand onto the panels that kicked dust off of the panels into suspension in the atmosphere, thereby increasing the power by ∼15% during this period. Final IDA activities included an indentation experiment that used the IDA scoop to push on the ground to measure the plastic deformation of the soil that complemented soil mechanics measurements from scoop interactions with the surface, and two experiments in which SEIS measured the tilt from the arm pressing on the ground to derive near surface elastic properties.

Title:	Sediment-moving winds and abrasion on Titan: Implications for yardangs
Authors:	MacKenzie, Shannon M.; Runyon, Kirby D.; Yu, Xinting; Kok, Jasper F.; Newman, Claire; Lorenz, Ralph D.; Comola, Francesco
Affiliation:	AA(Johns Hopkins University Applied Physics Laboratory, 1001 Johns Hopkins Road, Laurel, 20723, MD, USA), AB(Johns Hopkins University Applied Physics Laboratory, 1001 Johns Hopkins Road, Laurel, 20723, MD, USA; Planetary Sciences Institute, Tuscon, 85719-2395, AZ, USA), AC(Department of Earth and Planetary Sciences, University of California Santa Cruz, 1156 High Street, Santa Cruz, 95064, CA, USA), AD(Department of Atmospheric and Oceanic Sciences, University of California, Los Angeles, CA, USA), AE(Aeolis Research, Pasadena, 91107, CA, USA), AF(Johns Hopkins University Applied Physics Laboratory, 1001 Johns Hopkins Road, Laurel, 20723, MD, USA), AG(Department of Atmospheric and Oceanic Sciences, University of California, Los Angeles, CA, USA)
Journal:	Icarus, Volume 394, article id. 115433.
Publication Date:	Apr 2023
Origin:	Elsevier BV
Keywords:	Titan, Abrasion, Yardangs
Abstract Copyright:	(c) 2023 Elsevier Inc.
DOI:	https://doi.org/10.1016/j.icarus.2023.115433
Bibliographic Code:	2023Icar..39415433M
Abstract:	Titan's surface is expected to have a wide variety of sediments available due to both to aeolian and fluvial processes and to the organics that fall out of the atmosphere. As the vast dune fields that almost encircle Titan's equator indicate, Titan's near surface winds are sufficient to saltate particles. It is perhaps unsurprising then that putative yardangs - extended linear features carved by wind-mobilized sediment - have been found with Cassini RADAR data. However, few such candidates have been identified and are only found in the midlatitudes, a terrain whose geological characteristics (e.g. provenance, grain size distribution, composition) are still generally unknown. Therefore, to provide new insight into the possibility of yardang formation on Titan, we investigate the erodibility of Titan-relevant materials under plausible mid-latitude conditions. We found the most favorable conditions for abrasion in our study are created by small (≈ 100 μm diameter) particles with weak cohesion and weak (water-ice) targets; particle density is not a controlling factor.

Title:	Martian dust storm distribution and annual cycle from Mars daily global map observations
Authors:	Wang, Huiqun; Saidel, Morgan; Richardson, Mark I.; Toigo, Anthony D.; Battalio, J. Michael
Affiliation:	AA(Smithsonian Astrophysical Observatory, Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, USA), AB(Division of Geological and Planetary Sciences, Californian Institute of Technology, Pasadena, CA, USA), AC(Aeolis Research, Chandler, AZ, USA), AD(John Hopkins University Applied Physics Laboratory, Laurel, MD, USA), AE(Dept. Earth & Planetary Sci., Yale University, New Haven, CT, USA)
Journal:	Icarus, Volume 394, article id. 115416.
Publication Date:	Apr 2023
Origin:	Elsevier BV
Keywords:	Mars, atmosphere, climate, Atmospheres, composition, Meteorology
Abstract Copyright:	(c) 2023 Elsevier Inc.
DOI:	https://doi.org/10.1016/j.icarus.2022.115416
Bibliographic Code:	2023Icar..39415416W
Abstract:	Dust storms were manually tracked in Mars Reconnaissance Orbiter (MRO) Mars Daily Global Maps (MDGMs) from Mars Year 29 to 33. The data were used to construct the Mars Dust Storm Sequence Dataset (MDSSD), which contains >12,000 dust storm instances that are distinguishable from the ubiquitous dust background. Based on the dust storm climatology, we propose a partition of a Mars year into six pseudo-seasons or "sextons" (named "Unober", "Duober", "Triober", "Quartober", "Quintober", and "Sixtober", respectively). The greatest dust storm activity is observed in the 3rd, 4th and 6th sextons (Triober, Quartober and Sixtober), with each containing one or more dust storm episodes. We also propose a hierarchical system for organizing information and describing the process through which dust storms develop. The hierarchy of storm behavior is described in terms of dust storm episodes within these sextons, with each episode being composed of one or more dust storm sequences, and with each dust storm sequence being composed of multiple dust storm members. <P />The occurrence of a large dust storm episode typically results from multiple dust storm sequences that are simultaneous, staggered, or merged, though one of the component sequences typically plays a dominant role. The typical evolutionary pathway through which a large dust storm sequence develops consists of dust activity progressing from the northern to the southern hemispheres, with multiple flushing dust storm members in the northern hemisphere and followed by a much larger zonally extended dust storm member in the southern hemisphere. Differences among Mars years are related to the timing, order, and trajectories of dust storm sequences, though the overall spatial coverage of dust storm instances within a sexton is similar across years. A striking characteristic of Martian dust storm distribution is the quasi-periodic recurrence exhibited by dust storm episodes and dust storm sequences.

Title:	Near Surface Atmospheric Temperatures at Jezero From Mars 2020 MEDA Measurements
Authors:	Munguira, A.; Hueso, R.; Sánchez-Lavega, A.; de la Torre-Juarez, M.; Martínez, G. M.; Newman, C. E.; Sebastian, E.; Lepinette, A.; Vicente-Retortillo, A.; Chide, B.; Lemmon, M. T.; Bertrand, T.; Lorenz, R. D.; Banfield, D.; Gómez-Elvira, J.; Martín-Soler, J.; Navarro, S.; Pla-García, J.; Rodríguez-Manfredi, J. A.; Romeral, J.; Smith, M. D.; Torres, J.
Affiliation:	AA(Física Aplicada, Escuela de Ingeniería de Bilbao, Universidad del País Vasco UPV/EHU, Bilbao, Spain), AB(Física Aplicada, Escuela de Ingeniería de Bilbao, Universidad del País Vasco UPV/EHU, Bilbao, Spain), AC(Física Aplicada, Escuela de Ingeniería de Bilbao, Universidad del País Vasco UPV/EHU, Bilbao, Spain), AD(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AE(Lunar and Planetary Institute, Houston, TX USA), AF(Aeolis Research, Chandler, AZ USA), AG(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AH(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AI(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AJ(Los Alamos National Laboratory, Los Alamos, NM USA), AK(Space Science Institute, College Station, TX USA), AL(LESIA, Observatoire de Paris, Meudon, France), AM(Johns Hopkins Applied Physics Laboratory, Laurel, MD USA), AN(Cornell Center for Astrophysics and Planetary Science, Cornell University, Ithaca, NY USA), AO(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AP(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AQ(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AR(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AS(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AT(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AU(NASA Goddard Space Flight Center, Greenbelt, MD USA), AV(Centro de Astrobiología (INTA-CSIC), Madrid, Spain)
Journal:	Journal of Geophysical Research: Planets, Volume 128, Issue 3, article id. e2022JE007559.
Publication Date:	Mar 2023
Origin:	American Geophysical Union (AGU)
Keywords:	Mars, meteorology, planetary boundary layer, atmospheric temperatures, Mars 2020—Perseverance, MEDA
Abstract Copyright:	2023. American Geophysical Union. All Rights Reserved.
DOI:	https://doi.org/10.1029/2022JE007559
Bibliographic Code:	2023JGRE..12807559M
Abstract:	The Mars Environmental Dynamics Analyzer instrument on Mars 2020 has five Atmospheric Temperature Sensors at two altitudes (0.84 and 1.45 m) plus a Thermal InfraRed Sensor that measures temperatures on the surface and at ∼40 m. We analyze the measurements from these sensors to describe the evolution of temperatures in Jezero up to mission sol 400 (solar longitude L<SUB>S</SUB> = 13°-203°). The diurnal thermal cycle is characterized by a daytime convective period and a nocturnal stable atmosphere with a variable thermal inversion. We find a linear relationship between the daytime temperature fluctuations and the vertical thermal gradient with temperature fluctuations that peak at noon with typical values of 2.5 K at 1.45 m. In the late afternoon (∼17:00 Local True Solar Time), the atmosphere becomes vertically isothermal with vanishing fluctuations. We observe very small seasonal changes in air temperatures during the period analyzed. This is related to small changes in solar irradiation and dust opacity. However, we find significant changes in surface temperatures that are related to the variety of thermal inertias of the terrains explored along the traverse of Perseverance. These changes strongly influence the vertical thermal gradient, breaking the nighttime thermal inversion over terrains of high thermal inertia. We explore possible detections of atmospheric tides on near-surface temperatures and we examine variations in temperatures over timescales of a few sols that could be indicative of atmospheric waves affecting near-surface temperatures. We also discuss temperatures during a regional dust storm at L<SUB>S</SUB> = 153°-156° that simultaneously warmed the near surface atmosphere while cooling the surface.

Title:	Martian Wind and turbulence heard by the SuperCam microphone on the perseverance rover
Authors:	Stott, Alexander; Murdoch, Naomi; Gillier, Martin; Banfield, Don; Bertrand, Tanguy; Chide, Baptiste; De la Torre Juarez, Manuel; Hueso, Ricardo; Lorenz, Ralph; Martinez, German; Munguira, Asier; Mora Sotomayor, Luis; Navarro, Sara; Newman, Claire; Pilleri, Paolo; Pla-Garcia, Jorge; Randazzo, Nicolas; Rodriguez Manfredi, Jose Antonio; Sanchez-Lavega, Agustin; Smith, Michael; Viudez Moreiras, Daniel; Williams, Nathan; Maurice, Sylvestre; Wiens, Roger; Mimoun, David
Journal:	The Journal of the Acoustical Society of America, vol. 153, issue 3_supplement, pp. A279-A279.
Publication Date:	Mar 2023
Origin:	Acoustical Society of America (ASA)
DOI:	https://doi.org/10.1121/10.0018841
Bibliographic Code:	2023ASAJ..153A.279S
Abstract:	On top of listening to laser shots, rover sounds and the Ingenuity rotorcraft, SuperCam's Mars microphone has recorded over 7 hours of ambient background noise on Mars. These background recordings contain signal due to the Martian wind. Through a comparison to the meteorological data recorded by the MEDA (Mars Environmental Dynamics Analyzer), we can determine the relationships between the microphone data, the wind and the atmospheric stability. Based on these relationships, we have determined a way to estimate the wind speed using the microphone through Gaussian process regression, a machine learning technique. Owing to the sampling rate of 25 000 samples per second, the microphone data can be used to examine Mars' atmospheric dynamics at high frequencies, as yet unexplored on Mars. We will demonstrate how the wind speed estimates from the microphone provide an assessment of turbulence at fine scales, shedding light on the dissipative regime on Mars. One particularly interesting signal recorded by the microphone was a dust devil, which had fast varying winds within the walls of its vortex and signal from dust particles hitting the rover. Combining the microphone data with information from the MEDA sensors and navigation camera (Navcam) images enabled a full parameterization of this event.

Title:	Comparison of Ventifact Orientations and Recent Wind Direction Indicators on the Floor of Jezero Crater, Mars
Authors:	Herkenhoff, K. E.; Sullivan, R. J.; Newman, C. E.; Paar, G.; Baker, M.; Viúdez-Moreiras, D.; Ashley, J. W.; Bechtold, A.; Nuñez, J. I.
Affiliation:	AA(U.S. Geological Survey Astrogeology Science Center, Flagstaff, AZ USA), AB(Cornell University, Ithaca, NY USA), AC(Aeolis Research, Chandler, AZ USA), AD(Joanneum Research, Graz, Austria), AE(Smithsonian National Air and Space Museum, Washington, DC USA), AF(Centro de Astrobiologia, Madrid, Spain), AG(NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AH(University of Vienna, Vienna, Austria), AI(Applied Physics Laboratory, Johns Hopkins University, Laurel, MD USA)
Journal:	Journal of Geophysical Research: Planets, Volume 128, Issue 3, article id. e2022JE007599.
Publication Date:	Mar 2023
Origin:	American Geophysical Union (AGU)
Keywords:	Mars, ventifacts, climate, wind, Jezero, Perseverance
Abstract Copyright:	2023 Jet Propulsion Laboratory, California Institute of Technology and The Authors. Government sponsorship acknowledged. This article has been contributed to by U.S. Government employees and their work is in the public domain in the USA.
DOI:	https://doi.org/10.1029/2022JE007599
Bibliographic Code:	2023JGRE..12807599H
Abstract:	Wind-abraded rocks and aeolian bedforms have been observed at the Mars 2020 Perseverance landing site, providing evidence for recent and older wind directions. This study reports orientations of aeolian features measured in Perseverance images to infer formative wind directions. It compares these measurements with orbital observations, climate model predictions, and wind data acquired by the Mars Environmental Dynamics Analyzer. Three-dimensional orientations of flute textures on rocks, regolith wind tails extending from behind obstacles, and other aeolian features were measured using Digital Terrain Models derived from Mastcam-Z and navigation camera (Navcam) stereo images. Orientations of rock flutes measured in images acquired through Sol (Martian day) 400 yielded a mean azimuth of 94° ± 7° (wind from the west). However, similar measurements of regolith wind tails indicate that recent sand-driving winds have been blowing from the east-southeast, nearly the opposite direction (mean azimuth = 285° ± 15°). Atmospheric modeling generally predicts net annual sand transport from the east-southeast at present, consistent with Perseverance regolith wind tail and orbital observations. The orientation of ventifact flutes thus suggests that they were formed under a different climate regime. Differences in orientations of recent and paleo-wind indicators have been noted at other Mars landing sites and may result from major orbital/axial changes that can cause significant changes in atmospheric circulation. Orientation differences between modern and older wind direction indicators at Jezero are useful clues to the climate history of the region.

Title:	Surface Energy Budget, Albedo, and Thermal Inertia at Jezero Crater, Mars, as Observed From the Mars 2020 MEDA Instrument
Authors:	Martínez, G. M.; Sebastián, E.; Vicente-Retortillo, A.; Smith, M. D.; Johnson, J. R.; Fischer, E.; Savijärvi, H.; Toledo, D.; Hueso, R.; Mora-Sotomayor, L.; Gillespie, H.; Munguira, A.; Sánchez-Lavega, A.; Lemmon, M. T.; Gómez, F.; Polkko, J.; Mandon, L.; Apéstigue, V.; Arruego, I.; Ramos, M.; Conrad, P.; Newman, C. E.; Torre-Juarez, M. de la; Jordan, F.; Tamppari, L. K.; McConnochie, T. H.; Harri, A.-M.; Genzer, M.; Hieta, M.; Zorzano, M.-P.; Siegler, M.; Prieto, O.; Molina, A.; Rodríguez-Manfredi, J. A.
Affiliation:	AA(Lunar and Planetary Institute, Universities Space Research Association, Houston, TX USA; University of Michigan, Ann Arbor, MI USA), AB(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AC(University of Michigan, Ann Arbor, MI USA; Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AD(NASA Goddard Space Flight Center, Greenbelt, MD USA), AE(John Hopkins University Applied Physics Laboratory, Laurel, MD USA), AF(University of Michigan, Ann Arbor, MI USA), AG(University of Helsinki, Helsinki, Finland), AH(Instituto Nacional de Técnica Aeroespacial, Torrejón de Ardoz, Spain), AI(Universidad del País Vasco, Euskal Herriko Unibertsitatea, Leioa, Spain), AJ(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AK(Lunar and Planetary Institute, Universities Space Research Association, Houston, TX USA), AL(Universidad del País Vasco, Euskal Herriko Unibertsitatea, Leioa, Spain), AM(Universidad del País Vasco, Euskal Herriko Unibertsitatea, Leioa, Spain), AN(Space Science Institute, Boulder, CO USA), AO(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AP(Finnish Meteorological Institute, Helsink, Finland), AQ(Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris-PSL, Paris, France), AR(University of Helsinki, Helsinki, Finland), AS(University of Helsinki, Helsinki, Finland), AT(Universidad de Alcalá de Henares, Alcalá de Henares, Spain), AU(Carnegie Institution for Science, Washington, DC USA), AV(Aeolis Research, Chandler, AZ USA), AW(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AX(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AY(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AZ(Space Science Institute, Boulder, CO USA), BA(Finnish Meteorological Institute, Helsink, Finland), BB(Finnish Meteorological Institute, Helsink, Finland), BC(Finnish Meteorological Institute, Helsink, Finland), BD(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), BE(Planetary Science Institute, Tucson, AZ USA), BF(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), BG(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), BH(Centro de Astrobiología (INTA-CSIC), Madrid, Spain)
Journal:	Journal of Geophysical Research: Planets, Volume 128, Issue 2, article id. e2022JE007537.
Publication Date:	Feb 2023
Origin:	American Geophysical Union (AGU)
Keywords:	Mars, climate, surface, radiation, Mars 2020, albedo, thermal inertia
Abstract Copyright:	2023. American Geophysical Union. All Rights Reserved.
DOI:	https://doi.org/10.1029/2022JE007537
Bibliographic Code:	2023JGRE..12807537M
Abstract:	The Mars Environmental Dynamics Analyzer (MEDA) on board Perseverance includes first-of-its-kind sensors measuring the incident and reflected solar flux, the downwelling atmospheric IR flux, and the upwelling IR flux emitted by the surface. We use these measurements for the first 350 sols of the Mars 2020 mission (L<SUB>s</SUB> ∼ 6°-174° in Martian Year 36) to determine the surface radiative budget on Mars and to calculate the broadband albedo (0.3-3 μm) as a function of the illumination and viewing geometry. Together with MEDA measurements of ground temperature, we calculate the thermal inertia for homogeneous terrains without the need for numerical thermal models. We found that (a) the observed downwelling atmospheric IR flux is significantly lower than the model predictions. This is likely caused by the strong diurnal variation in aerosol opacity measured by MEDA, which is not accounted for by numerical models. (b) The albedo presents a marked non-Lambertian behavior, with lowest values near noon and highest values corresponding to low phase angles (i.e., Sun behind the observer). (c) Thermal inertia values ranged between 180 (sand dune) and 605 (bedrock-dominated material) SI units. (d) Averages of albedo and thermal inertia (spatial resolution of ∼3-4 m<SUP>2</SUP>) along Perseverance's traverse are in very good agreement with collocated retrievals of thermal inertia from Thermal Emission Imaging System (spatial resolution of 100 m per pixel) and of bolometric albedo in the 0.25-2.9 μm range from (spatial resolution of ∼300 km<SUP>2</SUP>). The results presented here are important to validate model predictions and provide ground-truth to orbital measurements.

Title:	Convective Vortices and Dust Devils Detected and Characterized by Mars 2020
Authors:	Hueso, R.; Newman, C. E.; del Río-Gaztelurrutia, T.; Munguira, A.; Sánchez-Lavega, A.; Toledo, D.; Apéstigue, V.; Arruego, I.; Vicente-Retortillo, A.; Martínez, G.; Lemmon, M.; Lorenz, R.; Richardson, M.; Viudez-Moreiras, D.; de la Torre-Juarez, M.; Rodríguez-Manfredi, J. A.; Tamppari, L. K.; Murdoch, N.; Navarro-López, S.; Gómez-Elvira, J.; Baker, M.; Pla-García, J.; Harri, A. M.; Hieta, M.; Genzer, M.; Polkko, J.; Jaakonaho, I.; Makinen, T.; Stott, A.; Mimoun, D.; Chide, B.; Sebastian, E.; Banfield, D.; Lepinette-Malvite, A.
Affiliation:	AA(Física Aplicada, Escuela de Ingeniería de Bilbao, Universidad del País Vasco UPV/EHU, Bilbao, Spain), AB(Aeolis Research, Chandler, AZ USA), AC(Física Aplicada, Escuela de Ingeniería de Bilbao, Universidad del País Vasco UPV/EHU, Bilbao, Spain), AD(Física Aplicada, Escuela de Ingeniería de Bilbao, Universidad del País Vasco UPV/EHU, Bilbao, Spain), AE(Física Aplicada, Escuela de Ingeniería de Bilbao, Universidad del País Vasco UPV/EHU, Bilbao, Spain), AF(Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain), AG(Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain), AH(Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain), AI(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AJ(Lunar and Planetary Institute, Houston, TX USA), AK(Space Science Institute, College Station, TX USA), AL(Johns Hopkins Applied Physics Laboratory, Laurel, MD USA), AM(Aeolis Research, Chandler, AZ USA), AN(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AO(Jet Propulsion Laboratory/California Institute of Technology, Pasadena, CA USA), AP(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AQ(Jet Propulsion Laboratory/California Institute of Technology, Pasadena, CA USA), AR(Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France), AS(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AT(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AU(Smithsonian Institution, Washington, DC USA), AV(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AW(Finnish Meteorological Institute, Helsinki, Finland), AX(Finnish Meteorological Institute, Helsinki, Finland), AY(Finnish Meteorological Institute, Helsinki, Finland), AZ(Finnish Meteorological Institute, Helsinki, Finland), BA(Finnish Meteorological Institute, Helsinki, Finland), BB(Finnish Meteorological Institute, Helsinki, Finland), BC(Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France), BD(Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France), BE(Los Alamos National Laboratory, Los Alamos, NM USA), BF(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), BG(Cornell Center for Astrophysics and Planetary Science, Cornell University, Ithaca, NY USA), BH(Centro de Astrobiología (INTA-CSIC), Madrid, Spain)
Journal:	Journal of Geophysical Research: Planets, Volume 128, Issue 2, article id. e2022JE007516.
Publication Date:	Feb 2023
Origin:	American Geophysical Union (AGU)
Keywords:	Mars, dust sevils, Jezero, MEDA
Abstract Copyright:	2023. The Authors.
DOI:	https://doi.org/10.1029/2022JE007516
Bibliographic Code:	2023JGRE..12807516H
Abstract:	We characterize vortex and dust devils (DDs) at Jezero from pressure and winds obtained with the Mars Environmental Dynamics Analyzer (MEDA) instrument on Mars 2020 over 415 Martian days (sols) (Ls = 6°-213°). Vortices are abundant (4.9 per sol with pressure drops >0.5 Pa correcting from gaps in coverage) and they peak at noon. At least one in every five vortices carries dust, and 75% of all vortices with ∆p > 2.0 Pa are dusty. Seasonal variability was small but DDs were abundant during a dust storm (Ls = 152°-156°). Vortices are more frequent and intense over terrains with lower thermal inertia favoring high daytime surface-to-air temperature gradients. We fit measurements of winds and pressure during DD encounters to models of vortices. We obtain vortex diameters that range from 5 to 135 m with a mean of 20 m, and from the frequency of close encounters we estimate a DD activity of 2.0-3.0 DDs km<SUP>-2</SUP> sol<SUP>-1</SUP>. A comparison of MEDA observations with a Large Eddy Simulation of Jezero at Ls = 45° produces a similar result. Three 100-m size DDs passed within 30 m of the rover from what we estimate that the activity of DDs with diameters >100 m is 0.1 DDs km<SUP>-2</SUP>sol<SUP>-1</SUP>, implying that dust lifting is dominated by the largest vortices in Jezero. At least one vortex had a central pressure drop of 9.0 Pa and internal winds of 25 ms<SUP>-1</SUP>. The MEDA wind sensors were partially damaged during two DD encounters whose characteristics we elaborate in detail.

Title:	Dynamical Core Damping of Thermal Tides in the Martian Atmosphere
Authors:	Lian, Yuan; Richardson, Mark I.; Newman, Claire E.; Lee, Chris; Toigo, Anthony; Guzewich, Scott; Yelle, Roger V.
Affiliation:	AA(Aeolis Research, Chandler, Arizona), AB(Aeolis Research, Chandler, Arizona), AC(Aeolis Research, Chandler, Arizona), AD(Aeolis Research, Chandler, Arizona; University of Toronto, Toronto, Ontario, Canada; University of Toronto, Toronto, Ontario, Canada), AE(The Johns Hopkins University, Baltimore, Maryland), AF(Goddard Space Flight Center, Greenbelt, Maryland), AG(The University of Arizona, Tucson, Arizona)
Journal:	Journal of the Atmospheric Sciences, Volume 80, Issue 2, p.535-547.
Publication Date:	Feb 2023
Origin:	American Meteorological Society
Abstract Copyright:	2023: American Meteorological Society
DOI:	https://doi.org/10.1175/JAS-D-22-0026.1
Bibliographic Code:	2023JAtS...80..535L
Abstract:	Atmospheric oscillations with daily periodicity are observed in in situ near-surface pressure, temperature, and winds observations and also in remotely sensed temperature and pressure observations of the Martian atmosphere. Such oscillations are interpreted as thermal tides driven by the diurnal cycle of solar radiation and occur at various frequencies, with the most prominent being the diurnal, semidiurnal, terdiurnal, and quadiurnal tides. Mars global circulation models reproduce these tides with varying levels of success. Until recently, both the MarsWRF and newly developed MarsMPAS models were able to produce realistic diurnal and semidiurnal tide amplitudes but predicted higher-order mode amplitudes that were significantly weaker than observed. We use linear wave analysis to show that the divergence damping applied within both MarsWRF and MarsMPAS is responsible for suppressing the amplitude of thermal tides with frequency greater than 2 per sol, despite being designed to suppress only acoustic wave modes. Decreasing the strength of the divergence damping in MarsWRF and MarsMPAS allows for excellent prediction of the higher-order tidal modes. This finding demonstrates that care must be taken when applying numerical dampers and filters that may eliminate some desired dynamical features in planetary atmospheres.

Title:	Dust Devil Frequency of Occurrence and Radiative Effects at Jezero Crater, Mars, as Measured by MEDA Radiation and Dust Sensor (RDS)
Authors:	Toledo, D.; Apéstigue, V.; Arruego, I.; Lemmon, M.; Gómez, L.; Montoro, F.; Hueso, R.; Newman, C.; Smith, M.; Viudez-Moreiras, D.; Martínez, G.; Lorenz, R.; Vicente-Retortillo, A.; Sanchez-Lavega, A.; Juarez, M. de la Torre; Rodriguez-Manfredi, J. A.; Carrasco, I.; Yela, M.; Jimenez, J. J.; García-Menendez, E.; Navarro, S.; Gomez-Elvira, F. J.; Harri, A.-M.; Polkko, J.; Hieta, M.; Genzer, M.; Murdoch, N.; Sebastian, E.
Affiliation:	AA(Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain), AB(Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain), AC(Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain), AD(Space Science Institute, Boulder, CO USA), AE(Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain), AF(Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain), AG(Universidad del País Vasco UPV/EHU, Bilbao, Spain), AH(Aeolis Research, Chandler, AZ USA), AI(NASA Godard Space Flight Center, Greenbelt, MD USA), AJ(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AK(Lunar and Planetary Institute, Universities Space Research Association, Houston, TX USA), AL(Johns Hopkins Applied Physics Laboratory, Laurel, MD USA), AM(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AN(Universidad del País Vasco UPV/EHU, Bilbao, Spain), AO(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AP(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AQ(Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain), AR(Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain), AS(Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain), AT(Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain), AU(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AV(Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain), AW(Finnish Meteorological Institute, Helsinki, Finland), AX(Finnish Meteorological Institute, Helsinki, Finland), AY(Finnish Meteorological Institute, Helsinki, Finland), AZ(Finnish Meteorological Institute, Helsinki, Finland), BA(Institut Supérieur de l'Aeronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France), BB(Centro de Astrobiología (INTA-CSIC), Madrid, Spain)
Journal:	Journal of Geophysical Research: Planets, Volume 128, Issue 1, article id. e2022JE007494.
Publication Date:	Jan 2023
Origin:	American Geophysical Union (AGU)
Keywords:	MEDA-RDS, dust devils, Mars 2020, dust
Abstract Copyright:	2023. The Authors.
DOI:	https://doi.org/10.1029/2022JE007494
Bibliographic Code:	2023JGRE..12807494T
Abstract:	The Mars Environmental Dynamics Analyzer, onboard the Perseverance rover, is a meteorological station that is operating on Mars and includes, among other sensors, the radiometer Radiation and Dust Sensor (RDS). From RDS irradiance observations, a total of 374 dust devils (DDs) were detected for the first 365 sols of the mission (Ls = 6°-182°), which along with wind and pressure measurements, we estimated a DD frequency of formation at Jezero between 1.3 and 3.4 DD km<SUP>-2</SUP> sol<SUP>-1</SUP> (increasing as we move from spring into summer). This frequency is found to be smaller than that estimated at the Spirit or Pathfinder landing sites but much greater than that derived at InSight landing site. The maximum in DD frequency occurs between 12:00 and 13:00 local true solar time, which is when the convective heat flux and lower planetary boundary layer IR heating are both predicted to peak in Jezero crater. DD diameter, minimum height, and trajectory were studied showing (a) an average diameter of 29 m (or a median of 25 m) and a maximum and minimum diameter of 132 ± 63.4 and 5.6 ± 5.5 m; (b) an average minimum DD height of 231 m and a maximum minimum-height of 872 m; and (c) the DD migration direction is in agreement with wind measurements. For all the cases, DDs decreased the UV irradiance, while at visible or near-IR wavelengths both increases and decreases were observed. Contrary to the frequency of formation, these results indicate similar DD characteristics in average for the studied period.

Title:	The diverse meteorology of Jezero crater over the first 250 sols of Perseverance on Mars
Authors:	Rodriguez-Manfredi, J. A.; de la Torre Juarez, M.; Sanchez-Lavega, A.; Hueso, R.; Martinez, G.; Lemmon, M. T.; Newman, C. E.; Munguira, A.; Hieta, M.; Tamppari, L. K.; Polkko, J.; Toledo, D.; Sebastian, E.; Smith, M. D.; Jaakonaho, I.; Genzer, M.; De Vicente-Retortillo, A.; Viudez-Moreiras, D.; Ramos, M.; Saiz-Lopez, A.; Lepinette, A.; Wolff, M.; Sullivan, R. J.; Gomez-Elvira, J.; Apestigue, V.; Conrad, P. G.; Del Rio-Gaztelurrutia, T.; Murdoch, N.; Arruego, I.; Banfield, D.; Boland, J.; Brown, A. J.; Ceballos, J.; Dominguez-Pumar, M.; Espejo, S.; Fairén, A. G.; Ferrandiz, R.; Fischer, E.; Garcia-Villadangos, M.; Gimenez, S.; Gomez-Gomez, F.; Guzewich, S. D.; Harri, A.-M.; Jimenez, J. J.; Jimenez, V.; Makinen, T.; Marin, M.; Martin, C.; Martin-Soler, J.; Molina, A.; Mora-Sotomayor, L.; Navarro, S.; Peinado, V.; Perez-Grande, I.; Pla-Garcia, J.; Postigo, M.; Prieto-Ballesteros, O.; Rafkin, S. C. R.; Richardson, M. I.; Romeral, J.; Romero, C.; Savijärvi, H.; Schofield, J. T.; Torres, J.; Urqui, R.; Zurita, S.; MEDA Team
Affiliation:	AA(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AB(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA), AC(Dept. Fí sica Aplicada, Universidad del País Vasco (UPV/EHU), Bilbaoí, Spain), AD(Dept. Fí sica Aplicada, Universidad del País Vasco (UPV/EHU), Bilbaoí, Spain), AE(Lunar and Planetary Institute, Houston, TX, USA), AF(Space Science Institute, Boulder, CO, USA), AG(Aeolis Corporation, Sierra Madre, CA, USA), AH(Dept. Fí sica Aplicada, Universidad del País Vasco (UPV/EHU), Bilbaoí, Spain), AI(Finnish Meteorological Institute, Helsinki, Finland), AJ(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA), AK(Finnish Meteorological Institute, Helsinki, Finland), AL(Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain), AM(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AN(NASA Goddard Space Flight Center, Greenbelt, MD, USA), AO(Finnish Meteorological Institute, Helsinki, Finland), AP(Finnish Meteorological Institute, Helsinki, Finland), AQ(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AR(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AS(Dept. Física y Matemáticas, Universidad de Alcalá, Alcalá de Henares, Spain), AT(Institute of Physical Chemistry Rocasolano, CSIC, Madrid, Spain), AU(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AV(Space Science Institute, Boulder, CO, USA), AW(Cornell University, Ithaca, NY, USA), AX(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AY(Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain), AZ(Carnegie Institution, Washington, DC, USA), BA(Dept. Fí sica Aplicada, Universidad del País Vasco (UPV/EHU), Bilbaoí, Spain), BB(Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France), BC(Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain), BD(NASA Ames Research Center, Mountain View, CA, USA), BE(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA), BF(Plancius Research, Severna Park, MD, USA), BG(Instituto de Microelectrónica de Sevilla (US-CSIC), Seville, Spain), BH(Dept. de Ingeniería Electrónica, Universidad Politécnica de Cataluña, Barcelona, Spain), BI(Instituto de Microelectrónica de Sevilla (US-CSIC), Seville, Spain), BJ(Centro de Astrobiología (INTA-CSIC), Madrid, Spain; Cornell University, Ithaca, NY, USA), BK(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), BL(Dept. of Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, MI, USA), BM(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), BN(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), BO(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), BP(NASA Goddard Space Flight Center, Greenbelt, MD, USA), BQ(Finnish Meteorological Institute, Helsinki, Finland), BR(Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain), BS(Dept. de Ingeniería Electrónica, Universidad Politécnica de Cataluña, Barcelona, Spain), BT(Finnish Meteorological Institute, Helsinki, Finland), BU(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), BV(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), BW(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), BX(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), BY(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), BZ(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), CA(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), CB(Dept. de Mecánica de Fluidos y Propulsión Aeroespacial, Universidad Politécnica de Madrid, Madrid, Spain), CC(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), CD(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), CE(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), CF(Southwest Research Institute, Boulder, CO, USA), CG(Aeolis Corporation, Sierra Madre, CA, USA), CH(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), CI(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), CJ(Finnish Meteorological Institute, Helsinki, Finland), CK(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA), CL(Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain), CM(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), CN(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), CO(Centro de Astrobiología (INTA-CSIC), Madrid, Spain; Dept. Física y Matemáticas, Universidad de Alcalá, Alcalá de Henares, Spain; Institute of Physical Chemistry Rocasolano, CSIC, Madrid, Spain; Cornell University, Ithaca, NY, USA; Carnegie Institution, Washington, DC, USA; Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France; NASA Ames Research Center, Mountain View, CA, USA; Plancius Research, Severna Park, MD, USA; Instituto de Microelectrónica de Sevilla (US-CSIC), Seville, Spain; Dept. de Ingeniería Electrónica, Universidad Politécnica de Cataluña, Barcelona, Spain; Dept. of Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, MI, USA; Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA; Dept. de Mecánica de Fluidos y Propulsión Aeroespacial, Universidad Politécnica de Madrid, Madrid, Spain; Southwest Research Institute, Boulder, CO, USA; Dept. Fí sica Aplicada, Universidad del País Vasco (UPV/EHU), Bilbaoí, Spain; Lunar and Planetary Institute, Houston, TX, USA; Space Science Institute, Boulder, CO, USA; Aeolis Corporation, Sierra Madre, CA, USA; Finnish Meteorological Institute, Helsinki, Finland; Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain; NASA Goddard Space Flight Center, Greenbelt, MD, USA)
Journal:	Nature Geoscience, Volume 16, Issue 1, p.19-28.
Publication Date:	Jan 2023
Origin:	Springer Science and Business Media LLC
DOI:	https://doi.org/10.1038/s41561-022-01084-0
Bibliographic Code:	2023NatGe..16...19R
Abstract:	NASA's Perseverance rover's Mars Environmental Dynamics Analyzer is collecting data at Jezero crater, characterizing the physical processes in the lowest layer of the Martian atmosphere. Here we present measurements from the instrument's first 250 sols of operation, revealing a spatially and temporally variable meteorology at Jezero. We find that temperature measurements at four heights capture the response of the atmospheric surface layer to multiple phenomena. We observe the transition from a stable night-time thermal inversion to a daytime, highly turbulent convective regime, with large vertical thermal gradients. Measurement of multiple daily optical depths suggests aerosol concentrations are higher in the morning than in the afternoon. Measured wind patterns are driven mainly by local topography, with a small contribution from regional winds. Daily and seasonal variability of relative humidity shows a complex hydrologic cycle. These observations suggest that changes in some local surface properties, such as surface albedo and thermal inertia, play an influential role. On a larger scale, surface pressure measurements show typical signatures of gravity waves and baroclinic eddies in a part of the seasonal cycle previously characterized as low wave activity. These observations, both combined and simultaneous, unveil the diversity of processes driving change on today's Martian surface at Jezero crater.

Title:	Mars 2020 Perseverance Rover Studies of the Martian Atmosphere Over Jezero From Pressure Measurements
Authors:	Sánchez-Lavega, A.; del Rio-Gaztelurrutia, T.; Hueso, R.; Juárez, M. de la Torre; Martínez, G. M.; Harri, A.-M.; Genzer, M.; Hieta, M.; Polkko, J.; Rodríguez-Manfredi, J. A.; Lemmon, M. T.; Pla-García, J.; Toledo, D.; Vicente-Retortillo, A.; Viúdez-Moreiras, D.; Munguira, A.; Tamppari, L. K.; Newman, C.; Gómez-Elvira, J.; Guzewich, S.; Bertrand, T.; Apéstigue, V.; Arruego, I.; Wolff, M.; Banfield, D.; Jaakonaho, I.; Mäkinen, T.
Affiliation:	AA(UPV/EHU, Bilbao, Spain), AB(UPV/EHU, Bilbao, Spain), AC(UPV/EHU, Bilbao, Spain), AD(Jet Propulsion Laboratory/California Institute of Technology, Pasadena, CA USA), AE(Lunar and Planetary Institute, Houston, TX USA), AF(Finnish Meteorological Institute, Helsinki, Finland), AG(Finnish Meteorological Institute, Helsinki, Finland), AH(Finnish Meteorological Institute, Helsinki, Finland), AI(Finnish Meteorological Institute, Helsinki, Finland), AJ(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AK(Space Science Institute, Boulder, CO USA), AL(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AM(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AN(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AO(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AP(UPV/EHU, Bilbao, Spain), AQ(Jet Propulsion Laboratory/California Institute of Technology, Pasadena, CA USA), AR(Aeolis Research, Pasadena, CA USA), AS(Instituto Nacional de Técnica Aeroespacial, INTA, Madrid, Spain), AT(NASA Goddard Space Flight Center, Greenbelt, MD USA), AU(Observatoire Paris Meudon, Paris, France), AV(Instituto Nacional de Técnica Aeroespacial, INTA, Madrid, Spain), AW(Instituto Nacional de Técnica Aeroespacial, INTA, Madrid, Spain), AX(Space Science Institute, Brookfield, WI USA), AY(Cornell University, Ithaca, NY USA), AZ(Finnish Meteorological Institute, Helsinki, Finland), BA(Finnish Meteorological Institute, Helsinki, Finland)
Journal:	Journal of Geophysical Research: Planets, Volume 128, Issue 1, article id. e2022JE007480.
Publication Date:	Jan 2023
Origin:	American Geophysical Union (AGU)
Keywords:	Mars atmosphere, pressure measurements, M2020 Perseverance, Astrophysics - Earth and Planetary Astrophysics
Abstract Copyright:	2022 The Authors.
DOI:	https://doi.org/10.1029/2022JE007480
Bibliographic Code:	2023JGRE..12807480S
Abstract:	The pressure sensors on Mars rover Perseverance measure the pressure field in the Jezero crater on regular hourly basis starting in sol 15 after landing. The present study extends up to sol 460 encompassing the range of solar longitudes from L<SUB>s</SUB> ∼ 13°-241° (Martian Year (MY) 36). The data show the changing daily pressure cycle, the sol-to-sol seasonal evolution of the mean pressure field driven by the CO<SUB>2</SUB> sublimation and deposition cycle at the poles, the characterization of up to six components of the atmospheric tides and their relationship to dust content in the atmosphere. They also show the presence of wave disturbances with periods 2-5 sols, exploring their baroclinic nature, short period oscillations (mainly at night-time) in the range 8-24 min that we interpret as internal gravity waves, transient pressure drops with duration ∼1-150 s produced by vortices, and rapid turbulent fluctuations. We also analyze the effects on pressure measurements produced by a regional dust storm over Jezero at L<SUB>s</SUB> ∼ 155°.

2022

Title:	The sound of a Martian dust devil
Authors:	Murdoch, N.; Stott, A. E.; Gillier, M.; Hueso, R.; Lemmon, M.; Martinez, G.; Apéstigue, V.; Toledo, D.; Lorenz, R. D.; Chide, B.; Munguira, A.; Sánchez-Lavega, A.; Vicente-Retortillo, A.; Newman, C. E.; Maurice, S.; de la Torre Juárez, M.; Bertrand, T.; Banfield, D.; Navarro, S.; Marin, M.; Torres, J.; Gomez-Elvira, J.; Jacob, X.; Cadu, A.; Sournac, A.; Rodriguez-Manfredi, J. A.; Wiens, R. C.; Mimoun, D.
Affiliation:	AA(Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France), AB(Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France), AC(Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France), AD(Física Aplicada, Escuela de Ingeniería de Bilbao, Universidad del País Vasco (UPV/EHU), Bilbao, Spain), AE(Space Science Institute, 80301, Boulder, CO, USA), AF(Lunar and Planetary Institute, Universities Space Research Association, Houston, TX, USA; Department of Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, MI, USA), AG(Instituto Nacional de Técnica Aeroespacial, Madrid, Spain), AH(Instituto Nacional de Técnica Aeroespacial, Madrid, Spain), AI(Space Exploration Sector, Johns Hopkins Applied Physics Laboratory, Laurel, MD, USA), AJ(Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA), AK(Física Aplicada, Escuela de Ingeniería de Bilbao, Universidad del País Vasco (UPV/EHU), Bilbao, Spain), AL(Física Aplicada, Escuela de Ingeniería de Bilbao, Universidad del País Vasco (UPV/EHU), Bilbao, Spain), AM(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AN(Aeolis Research, Chandler, AZ, USA), AO(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France), AP(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA), AQ(Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique (LESIA), Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Univ. Paris Diderot, Sorbonne Paris Cité, 5 place Jules Janssen, 92195, Meudon, France), AR(Cornell University, Ithaca, NY, USA; NASA AMES Research Center, Moffett Field, CA, USA), AS(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AT(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AU(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AV(Instituto Nacional de Técnica Aeroespacial, Madrid, Spain), AW(Institut de Mécanique des Fluides, Université de Toulouse III Paul Sabatier, INP, CNRS, Toulouse, France), AX(Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France), AY(Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France), AZ(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), BA(Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN, USA), BB(Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France)
Journal:	Nature Communications, Volume 13, article id. 7505.
Publication Date:	Dec 2022
Origin:	Springer Science and Business Media LLC
DOI:	https://doi.org/10.1038/s41467-022-35100-z
Bibliographic Code:	2022NatCo..13.7505M
Abstract:	Dust devils (convective vortices loaded with dust) are common at the surface of Mars, particularly at Jezero crater, the landing site of the Perseverance rover. They are indicators of atmospheric turbulence and are an important lifting mechanism for the Martian dust cycle. Improving our understanding of dust lifting and atmospheric transport is key for accurate simulation of the dust cycle and for the prediction of dust storms, in addition to being important for future space exploration as grain impacts are implicated in the degradation of hardware on the surface of Mars. Here we describe the sound of a Martian dust devil as recorded by the SuperCam instrument on the Perseverance rover. The dust devil encounter was also simultaneously imaged by the Perseverance rover's Navigation Camera and observed by several sensors in the Mars Environmental Dynamics Analyzer instrument. Combining these unique multi-sensorial data with modelling, we show that the dust devil was around 25 m large, at least 118 m tall, and passed directly over the rover travelling at approximately 5 m s<SUP>‒1</SUP>. Acoustic signals of grain impacts recorded during the vortex encounter provide quantitative information about the number density of particles in the vortex. The sound of a Martian dust devil was inaccessible until SuperCam microphone recordings. This chance dust devil encounter demonstrates the potential of acoustic data for resolving the rapid wind structure of the Martian atmosphere and for directly quantifying wind-blown grain fluxes on Mars.

Title:	Winds at the Mars 2020 Landing Site: 1. Near-Surface Wind Patterns at Jezero Crater
Authors:	Viúdez-Moreiras, D.; Lemmon, M.; Newman, C. E.; Guzewich, S.; Mischna, M.; Gómez-Elvira, J.; Herkenhoff, K.; Sánchez-Lavega, A.; de la Torre, M.; Rodríguez-Manfredi, J. A.; Lorenz, R. D.; Pla-García, J.; Hueso, R.; Richardson, M.; Tamppari, L.; Smith, M.; Apéstigue, V.; Toledo, D.; Bell, J.
Affiliation:	AA(Centro de Astrobiologia (CAB, CSIC-INTA) and National Institute for Aerospace Technology (INTA), Madrid, Spain), AB(Space Science Institute, College Station, TX USA), AC(Aeolis Research, Chandler, AZ USA), AD(NASA Goddard Spaceflight Center, Greenbelt, MD USA), AE(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AF(National Institute for Aerospace Technology (INTA), Madrid, Spain), AG(USGS Astrogeology Science Center, Flagstaff, AZ USA), AH(Universidad del País Vasco (UPV/EHU), Bilbao, Spain), AI(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AJ(Centro de Astrobiologia (CAB, CSIC-INTA) and National Institute for Aerospace Technology (INTA), Madrid, Spain), AK(Johns Hopkins University Applied Physics Laboratory, Laurel, MD USA), AL(Centro de Astrobiologia (CAB, CSIC-INTA) and National Institute for Aerospace Technology (INTA), Madrid, Spain), AM(USGS Astrogeology Science Center, Flagstaff, AZ USA), AN(Aeolis Research, Chandler, AZ USA), AO(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AP(NASA Goddard Spaceflight Center, Greenbelt, MD USA), AQ(National Institute for Aerospace Technology (INTA), Madrid, Spain), AR(National Institute for Aerospace Technology (INTA), Madrid, Spain), AS(School of Earth and Space Exploration, Arizona State University, Tempe, AZ USA)
Journal:	Journal of Geophysical Research: Planets, Volume 127, Issue 12, article id. e2022JE007522.
Publication Date:	Dec 2022
Origin:	American Geophysical Union (AGU)
Abstract Copyright:	2022. The Authors.
DOI:	https://doi.org/10.1029/2022JE007522
Bibliographic Code:	2022JGRE..12707522V
Abstract:	This is the first part of a two-part paper. NASA's Mars 2020 Perseverance rover measured winds on the Jezero crater floor close to the delta of an ancient river. A mostly repeatable diurnal cycle was observed and presented two regimes: (a) a convective regime, from dawn to sunset, with average easterly to southeasterly winds, during which maximum wind speeds were measured, and (b) a nighttime regime with westerly-northwesterly winds followed by a relatively calm period with highly variable wind directions as a function of sol and time of night. The timing and magnitude of the observed regimes are consistent with primary control by regional and local slope flows. Data suggest that the surface circulation at Jezero region in northern spring and summer is highly unaffected by large-scale circulation except during particular periods in the diurnal cycle or generally during dust storms, which is supported by MarsWRF model simulations. Consequently, the observed seasonal variability was weak. However, sol-to-sol and seasonal variability were measured, most of it during certain nighttime periods. Traveling waves consistent with baroclinic instability were clearly observed in surface winds at L<SUB>s</SUB> ∼ 75°. The early MY36/2022A regional dust storm at L<SUB>s</SUB> ∼ 153° disturbed the wind patterns with changes suggesting enhanced tidal flows. After sunset, the dust storm also produced detectable gravity wave activity, increasing the mixing in the nighttime planetary boundary layer during storm conditions. Inferred wind directions from dust devil movies strongly suggest that prevailing winds continued to be slope-driven during the late summer, fall and early winter seasons.

Title:	Lifting and Transport of Martian Dust by the Ingenuity Helicopter Rotor Downwash as Observed by High-Speed Imaging From the Perseverance Rover
Authors:	Lemmon, M. T.; Lorenz, R. D.; Rabinovitch, J.; Newman, C. E.; Williams, N. R.; Sullivan, R.; Golombek, M. P.; Bell, J. F.; Maki, J. N.; Vicente-Retortillo, A.
Affiliation:	AA(Space Science Institute, Boulder, CO USA), AB(Applied Physics Laboratory, Laurel, MD USA), AC(Stevens Institute of Technology, Hoboken, NJ USA), AD(Aeolis Research, Chandler, AZ USA), AE(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AF(Cornell University, Ithaca, NY USA), AG(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AH(Arizona State University, Tempe, AZ USA), AI(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AJ(Centro de Astrobiologia (INTA-CSIC), Madrid, Spain)
Journal:	Journal of Geophysical Research: Planets, Volume 127, Issue 12, article id. e2022JE007605.
Publication Date:	Dec 2022
Origin:	American Geophysical Union (AGU)
Keywords:	Mars, dust, helicopter, Perseverance, Ingenuity
Abstract Copyright:	2022. The Authors.
DOI:	https://doi.org/10.1029/2022JE007605
Bibliographic Code:	2022JGRE..12707605L
Abstract:	Martian atmospheric dust is a major driver of weather, with feedback between atmospheric dust distribution, circulation changes from radiative heating and cooling driven by this dust, and winds that mobilize surface dust and distribute it in the atmosphere. Wind-driven mobilization of surface dust is a poorly understood process due to significant uncertainty about minimum wind stress and whether the saltation of sand particles is required. This study utilizes video of six Ingenuity helicopter flights to measure dust lifting during helicopter ascents, traverses, and descents. Dust mobilization persisted on takeoff until the helicopter exceeded 3 m altitude, with dust advecting at 4-6 m/s. During landing, dust mobilization initiated at 2.3-3.6 m altitude. Extensive dust mobilization occurred during traverses at 5.1-5.7 m altitude. Dust mobilization threshold friction velocity of rotor-induced winds during landing is modeled at 0.4-0.6 m/s (factor of two uncertainty in this estimate), with higher winds required when the helicopter was over undisturbed terrain. Modeling dust mobilization from >5 m cruising altitude indicates mobilization by 0.3 m/s winds, suggesting nonsaltation mechanisms such as mobilization and destruction of dust aggregates. No dependence on background winds was seen for the initiation of dust lifting but one case of takeoff in 7 m/s winds created a track of darkened terrain downwind of the helicopter, which may have been a saltation cluster. When the helicopter was cruising at 5-6 m altitude, recirculation was seen in the dust clouds.

Title:	Science goals and new mission concepts for future exploration of Titan's atmosphere, geology and habitability: titan POlar scout/orbitEr and in situ lake lander and DrONe explorer (POSEIDON)
Authors:	Rodriguez, Sébastien; Vinatier, Sandrine; Cordier, Daniel; Tobie, Gabriel; Achterberg, Richard K.; Anderson, Carrie M.; Badman, Sarah V.; Barnes, Jason W.; Barth, Erika L.; Bézard, Bruno; Carrasco, Nathalie; Charnay, Benjamin; Clark, Roger N.; Coll, Patrice; Cornet, Thomas; Coustenis, Athena; Couturier-Tamburelli, Isabelle; Dobrijevic, Michel; Flasar, F. Michael; de Kok, Remco; Freissinet, Caroline; Galand, Marina; Gautier, Thomas; Geppert, Wolf D.; Griffith, Caitlin A.; Gudipati, Murthy S.; Hadid, Lina Z.; Hayes, Alexander G.; Hendrix, Amanda R.; Jaumann, Ralf; Jennings, Donald E.; Jolly, Antoine; Kalousova, Klara; Koskinen, Tommi T.; Lavvas, Panayotis; Lebonnois, Sébastien; Lebreton, Jean-Pierre; Le Gall, Alice; Lellouch, Emmanuel; Le Mouélic, Stéphane; Lopes, Rosaly M. C.; Lora, Juan M.; Lorenz, Ralph D.; Lucas, Antoine; MacKenzie, Shannon; Malaska, Michael J.; Mandt, Kathleen; Mastrogiuseppe, Marco; Newman, Claire E.; Nixon, Conor A.; Radebaugh, Jani; Rafkin, Scot C.; Rannou, Pascal; Sciamma-O'Brien, Ella M.; Soderblom, Jason M.; Solomonidou, Anezina; Sotin, Christophe; Stephan, Katrin; Strobel, Darrell; Szopa, Cyril; Teanby, Nicholas A.; Turtle, Elizabeth P.; Vuitton, Véronique; West, Robert A.
Affiliation:	AA(Université de Paris, Institut de physique du globe de Paris, CNRS, F-75005, Paris, France), AB(LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, niversité de Paris, 5 place Jules Janssen, 92195, Meudon, France), AC(Groupe de Spectrométrie Moléculaire et Atmosphérique, UMR CNRS 7331, Université de Reims Champagne-Ardenne, Reims, France), AD(Laboratoire de Planétologie et Géodynamique, UMR 6112, CNRS, Université de Nantes, 2 rue de la Houssinière, 44322, Nantes, France), AE(Department of Astronomy, University of Maryland, 20742, College Park, MD, USA), AF(Planetary Systems Laboratory, NASA Goddard Space Flight Center, 20771, Greenbelt, MD, USA), AG(Department of Physics and Astronomy, University of Leicester, Leicester, UK), AH(Department of Physics, University of Idaho, Moscow, ID, USA), AI(Southwest Research Institute, Boulder, CO, USA), AJ(LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, niversité de Paris, 5 place Jules Janssen, 92195, Meudon, France), AK(LATMOS/IPSL, UVSQ Université Paris-Saclay, Sorbonne Université, CNRS, Paris, France), AL(LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, niversité de Paris, 5 place Jules Janssen, 92195, Meudon, France), AM(Planetary Science Institute Colorado, 1546 Cole Blvd #120, 80401, Lakewood, CO, USA), AN(LISA, Université Paris-Est, Creteil, France), AO(Aurora Technology BV for ESA - European Space Agency, European Space Astronomy Centre (ESAC), Camino Bajo del Castillo s/n, Villanueva de la Cañada, 28692, Madrid, Spain), AP(LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, niversité de Paris, 5 place Jules Janssen, 92195, Meudon, France), AQ(Aix-Marseille Université, CNRS, PIIM, UMR 7345, 13013, Marseille, France), AR(Laboratoire d'Astrophysique de Bordeaux, Université Bordeaux, CNRS, B18N, allée Geoffroy Saint-Hilaire, 33615, Pessac, France), AS(Planetary Systems Laboratory, NASA Goddard Space Flight Center, 20771, Greenbelt, MD, USA), AT(Department of Physical Geography, Utrecht University, Utrecht, Netherlands), AU(LATMOS/IPSL, UVSQ Université Paris-Saclay, Sorbonne Université, CNRS, Paris, France), AV(Department of Physics, Imperial College London, Prince Consort Road, SW7 2AZ, London, UK), AW(LATMOS/IPSL, UVSQ Université Paris-Saclay, Sorbonne Université, CNRS, Paris, France), AX(Department of Physics, AlbaNova University Center, Stockholm University, Roslagstullsbacken 21, SE-10691, Stockholm, Sweden), AY(Lunar and Planetary Laboratory, University of Arizona, 1629 E. University Blvd., 85721, Tucson, AZ, USA), AZ(Jet Propulsion Laboratory, Caltech, 4800 Oak Grove Drive, 91109, Pasadena, CA, USA), BA(Laboratoire de Physique des Plasmas (LPP), CNRS, Observatoire de Paris, Sorbonne Université, Université Paris Saclay, Ecole polytechnique, Institut Polytechnique de Paris, 91120, Palaiseau, France), BB(Cornell University, Ithaca, NY, USA), BC(Planetary Science Institute Colorado, 1546 Cole Blvd #120, 80401, Lakewood, CO, USA), BD(Institute of Geological Sciences, Free University Berlin, Berlin, Germany), BE(Planetary Systems Laboratory, NASA Goddard Space Flight Center, 20771, Greenbelt, MD, USA), BF(LISA, Université Paris-Est, Creteil, France), BG(Faculty of Mathematics and Physics, Department of Geophysics, Charles University, Prague, Czech Republic), BH(Lunar and Planetary Laboratory, University of Arizona, 1629 E. University Blvd., 85721, Tucson, AZ, USA), BI(Groupe de Spectrométrie Moléculaire et Atmosphérique, UMR CNRS 7331, Université de Reims Champagne-Ardenne, Reims, France), BJ(Laboratoire de Météorologie Dynamique (LMD/IPSL), Sorbonne Université, ENS, PSL Research University, Ecole Polytechnique, Institut Polytechnique de Paris, CNRS, Paris, France), BK(Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), UMR 7328 CNRS, Université d'Orléans, Orléans, France), BL(LATMOS/IPSL, UVSQ Université Paris-Saclay, Sorbonne Université, CNRS, Paris, France), BM(LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, niversité de Paris, 5 place Jules Janssen, 92195, Meudon, France), BN(Laboratoire de Planétologie et Géodynamique, UMR 6112, CNRS, Université de Nantes, 2 rue de la Houssinière, 44322, Nantes, France), BO(Jet Propulsion Laboratory, Caltech, 4800 Oak Grove Drive, 91109, Pasadena, CA, USA), BP(Department of Earth and Planetary Sciences, Yale University, 210 Whitney Avenue, 06511, New Haven, CT, USA), BQ(Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Rd., 20723, Laurel, MD, USA), BR(Université de Paris, Institut de physique du globe de Paris, CNRS, F-75005, Paris, France), BS(Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Rd., 20723, Laurel, MD, USA), BT(Jet Propulsion Laboratory, Caltech, 4800 Oak Grove Drive, 91109, Pasadena, CA, USA), BU(Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Rd., 20723, Laurel, MD, USA), BV("La Sapienza" University of Rome, Rome, Italy), BW(Aeolis Research, 333 N. Dobson Road, Unit 5, 85224, Chandler, AZ, USA), BX(Planetary Systems Laboratory, NASA Goddard Space Flight Center, 20771, Greenbelt, MD, USA), BY(Department of Geological Sciences, Brigham Young University, S-389 ESC, 84602, Provo, UT, USA), BZ(Southwest Research Institute, Boulder, CO, USA), CA(Groupe de Spectrométrie Moléculaire et Atmosphérique, UMR CNRS 7331, Université de Reims Champagne-Ardenne, Reims, France), CB(Space Science and Astrobiology Division, NASA Ames Research Center, 94035, Moffett Field, CA, USA), CC(Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA), CD(Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA, USA), CE(Laboratoire de Planétologie et Géodynamique, UMR 6112, CNRS, Université de Nantes, 2 rue de la Houssinière, 44322, Nantes, France), CF(DLR, Institute of Planetary Research, Berlin, Germany), CG(The Johns Hopkins University, Baltimore, MD, USA), CH(LATMOS/IPSL, UVSQ Université Paris-Saclay, Sorbonne Université, CNRS, Paris, France), CI(School of Earth Sciences, University of Bristol, Wills Memorial Building, Queens Road, BS8 1RJ, Bristol, UK), CJ(Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Rd., 20723, Laurel, MD, USA), CK(Univ. Grenoble Alpes, CNRS, IPAG, 38000, Grenoble, France), CL(Jet Propulsion Laboratory, Caltech, 4800 Oak Grove Drive, 91109, Pasadena, CA, USA)
Journal:	Experimental Astronomy, Volume 54, Issue 2-3, p.911-973.
Publication Date:	Dec 2022
Origin:	Springer Science and Business Media LLC
Keywords:	Titan, Atmosphere, Geology, Habitability, Orbiter, Lake lander, Drones, Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
DOI:	https://doi.org/10.1007/s10686-021-09815-8
Bibliographic Code:	2022ExA....54..911R
Abstract:	In response to ESA's "Voyage 2050" announcement of opportunity, we propose an ambitious L-class mission to explore one of the most exciting bodies in the Solar System, Saturn's largest moon Titan. Titan, a "world with two oceans", is an organic-rich body with interior-surface-atmosphere interactions that are comparable in complexity to the Earth. Titan is also one of the few places in the Solar System with habitability potential. Titan's remarkable nature was only partly revealed by the Cassini-Huygens mission and still holds mysteries requiring a complete exploration using a variety of vehicles and instruments. The proposed mission concept POSEIDON (Titan POlar Scout/orbitEr and In situ lake lander DrONe explorer) would perform joint orbital and in situ investigations of Titan. It is designed to build on and exceed the scope and scientific/technological accomplishments of Cassini-Huygens, exploring Titan in ways that were not previously possible, in particular through full close-up and in situ coverage over long periods of time. In the proposed mission architecture, POSEIDON consists of two major elements: a spacecraft with a large set of instruments that would orbit Titan, preferably in a low-eccentricity polar orbit, and a suite of in situ investigation components, i.e. a lake lander, a "heavy" drone (possibly amphibious) and/or a fleet of mini-drones, dedicated to the exploration of the polar regions. The ideal arrival time at Titan would be slightly before the next northern Spring equinox (2039), as equinoxes are the most active periods to monitor still largely unknown atmospheric and surface seasonal changes. The exploration of Titan's northern latitudes with an orbiter and in situ element(s) would be highly complementary in terms of timing (with possible mission timing overlap), locations, and science goals with the upcoming NASA New Frontiers Dragonfly mission that will provide in situ exploration of Titan's equatorial regions, in the mid-2030s.

Title:	Winds at the Mars 2020 Landing Site. 2. Wind Variability and Turbulence
Authors:	Viúdez-Moreiras, D.; de la Torre, M.; Gómez-Elvira, J.; Lorenz, R. D.; Apéstigue, V.; Guzewich, S.; Mischna, M.; Sullivan, R.; Herkenhoff, K.; Toledo, D.; Lemmon, M.; Smith, M.; Newman, C. E.; Sánchez-Lavega, A.; Rodríguez-Manfredi, J. A.; Richardson, M.; Hueso, R.; Harri, A. M.; Tamppari, L.; Arruego, I.; Bell, J.
Affiliation:	AA(Centro de Astrobiología (CAB, CSIC-INTA) and National Institute for Aerospace Technology (INTA), Madrid, Spain), AB(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AC(National Institute for Aerospace Technology (INTA), Madrid, Spain), AD(Johns Hopkins Applied Physics Lab, Laurel, MD USA), AE(National Institute for Aerospace Technology (INTA), Madrid, Spain), AF(NASA Goddard Spaceflight Center, Greenbelt, MD USA), AG(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AH(Cornell University, Ithaca, NY USA), AI(USGS Astrogeology Science Center, Flagstaff, AZ USA), AJ(National Institute for Aerospace Technology (INTA), Madrid, Spain), AK(Space Science Institute, College Station, TX USA), AL(NASA Goddard Spaceflight Center, Greenbelt, MD USA), AM(Aeolis Research, Chandler, AZ USA), AN(Universidad del País Vasco (UPV/EHU), Bilbao, Spain), AO(Centro de Astrobiología (CAB, CSIC-INTA) and National Institute for Aerospace Technology (INTA), Madrid, Spain), AP(Aeolis Research, Chandler, AZ USA), AQ(Universidad del País Vasco (UPV/EHU), Bilbao, Spain), AR(Finnish Meteorological Institute, Helsinki, Finland), AS(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AT(National Institute for Aerospace Technology (INTA), Madrid, Spain), AU(School of Earth and Space Exploration, Arizona State University, Tempe, AZ USA)
Journal:	Journal of Geophysical Research: Planets, Volume 127, Issue 12, article id. e2022JE007523.
Publication Date:	Dec 2022
Origin:	American Geophysical Union (AGU)
Abstract Copyright:	2022. The Authors.
DOI:	https://doi.org/10.1029/2022JE007523
Bibliographic Code:	2022JGRE..12707523V
Abstract:	Wind speeds measured by the Mars 2020 Perseverance rover in Jezero crater were fitted as a Weibull distribution. InSight wind data acquired in Elysium Planitia were also used to contextualize observations. Jezero winds were found to be much calmer on average than in previous landing sites, despite the intense aeolian activity observed. However, a great influence of turbulence and wave activity was observed in the wind speed variations, thus driving the probability of reaching the highest wind speeds at Jezero, instead of sustained winds driven by local, regional, or large-scale circulation. The power spectral density of wind speed fluctuations follows a power-law, whose slope deviates depending on the time of day from that predicted considering homogeneous and isotropic turbulence. Daytime wave activity is related to convection cells and smaller eddies in the boundary layer, advected over the crater. The signature of convection cells was also found during dust storm conditions, when prevailing winds were consistent with a tidal drive. Nighttime fluctuations were also intense, suggesting strong mechanical turbulence. Convective vortices were usually involved in rapid wind fluctuations and extreme winds, with variations peaking at 9.2 times the background winds. Transient high wind events by vortex-passages, turbulence, and wave activity could be driving aeolian activity at Jezero. We report the detection of a strong dust cloud of 0.75-1.5 km in length passing over the rover. The observed aeolian activity had major implications for instrumentation, with the wind sensor suffering damage throughout the mission, probably due to flying debris advected by winds.

Title:	Acoustics Reveals Short-Term Air Temperature Fluctuations Near Mars' Surface
Authors:	Chide, Baptiste; Bertrand, Tanguy; Lorenz, Ralph D.; Munguira, Asier; Hueso, Ricardo; Sánchez-Lavega, Agustin; Martinez, German; Spiga, Aymeric; Jacob, Xavier; de la Torre Juarez, Manuel; Lemmon, Mark T.; Banfield, Don; Newman, Claire E.; Murdoch, Naomi; Stott, Alexander; Viúdez-Moreiras, Daniel; Pla-Garcia, Jorge; Larmat, Carène; Lanza, Nina L.; Rodríguez-Manfredi, José Antonio; Wiens, Roger C.
Affiliation:	AA(Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM USA), AB(LESIA, Observatoire de Paris, Université PSL, Sorbonne Université, Université de Paris, CNRS, Meudon, France), AC(Space Exploration Sector, Johns Hopkins Applied Physics Laboratory, Laurel, MD USA), AD(Física Aplicada, Escuela de Ingeniería de Bilbao, UPV/EHU, Bilbao, Spain), AE(Física Aplicada, Escuela de Ingeniería de Bilbao, UPV/EHU, Bilbao, Spain), AF(Física Aplicada, Escuela de Ingeniería de Bilbao, UPV/EHU, Bilbao, Spain), AG(Lunar and Planetary Institute, Universities Space Research Association, Houston, TX USA; Department of Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, MI USA), AH(Laboratoire de Météorologie Dynamique (LMD), Institut Pierre-Simon Laplace (IPSL), Sorbonne Université, Centre National de la Recherche Scientifique (CNRS), École Polytechnique, École Normale Supérieure (ENS), Paris, France; Institut Universitaire de France, Paris, France), AI(Institut de Mécanique des Fluides de Toulouse, Université de Toulouse III Paul Sabatier, INP, CNRS, Toulouse, France), AJ(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AK(Space Science Institute, Boulder, CO USA), AL(NASA Ames Research Center, Mountain View, CA USA), AM(Aeolis Research, Chandler, AZ USA), AN(Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France), AO(Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France), AP(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AQ(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AR(Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM USA), AS(Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM USA), AT(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AU(Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN USA)
Journal:	Geophysical Research Letters, Volume 49, Issue 21, article id. e2022GL100333.
Publication Date:	Nov 2022
Origin:	American Geophysical Union (AGU)
Keywords:	Mars atmosphere, temperature fluctuations, acoustics, turbulence
Abstract Copyright:	2022. The Authors.
DOI:	https://doi.org/10.1029/2022GL100333
Bibliographic Code:	2022GeoRL..4900333C
Abstract:	Acoustics is new on Mars: it allows the characterization of turbulence at smaller scales than previously possible within the lowest part of the Planetary Boundary Layer. Sound speed measurements, by the SuperCam instrument and its microphone onboard the NASA Perseverance rover, allow the retrieval of atmospheric temperatures at 0.77 m above the ground, at 3 Hz, with a ∼10 ms response time that is 20-100 times shorter than for typical thermocouple sensors used on Mars. Here we report on the first measurements of the sound speed-derived temperature and its fluctuations near the surface. Data highlight large and rapid fluctuations up to ±7 K/s, whose amplitude over such a timescale has never been reported, nor predicted by atmospheric models. These fluctuations follow the daytime pattern of the turbulence and highlight occasional high amplitude events that are likely due to the conjunction of low thermal inertia and strong winds.

Title:	Planetary Waves Traveling Between Mars Science Laboratory and Mars 2020
Authors:	Battalio, J. Michael; Martínez, Germán.; Newman, Claire; de la Torre Juarez, Manuel; Sánchez-Lavega, Agustín.; Víudez-Moreiras, Daniel
Affiliation:	AA(Department of Earth and Planetary Sciences, Yale University, New Haven, CT USA), AB(Lunar and Planetary Institute, USRA, Houston, TX USA), AC(Aeolis Research, Pasadena, CA USA), AD(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AE(Departamento Física Aplicada I, Universidad del País Vasco UPV/EHU, Bilbao, Spain), AF(Centro de Astrobiología (INTA-CSIC), Madrid, Spain)
Journal:	Geophysical Research Letters, Volume 49, Issue 21, article id. e2022GL100866.
Publication Date:	Nov 2022
Origin:	American Geophysical Union (AGU)
Keywords:	Mars, planetary waves, Mars Science Laboratory, Mars 2020, reanalysis
Abstract Copyright:	2022. American Geophysical Union. All Rights Reserved.
DOI:	https://doi.org/10.1029/2022GL100866
Bibliographic Code:	2022GeoRL..4900866B
Abstract:	Using Perseverance (Mars 2020) and Mars Science Laboratory (MSL) measurements, we obtain planetary waves with a period of 1.5-30 sols in the 1.5 m temperature, winds (Mars 2020), surface pressure, and relative humidity. Planetary waves emerge and propagate latitudinally across all variables. Short-period waves peak at periods of ∼2, 3, and 4.5 sols, confirming previous detections of waves, and wave amplitudes agree at Mars 2020 and MSL for all variables. The simultaneous detection of waves within Gale and Jezero craters in multiple variables indicates that planetary-scale dynamics influences many facets of local weather throughout the year. Multiple waves are correlated or anti-correlated between MSL and Mars 2020, suggesting waves originate in both hemispheres. Further, waves at one site do not always lead the other, suggesting a combination of baroclinic and barotropic processes as wave sources, determined from the phasing of the temperature and winds in Jezero compared to the Ensemble Mars Atmospheric Reanalysis System.

Title:	Dust, Sand, and Winds Within an Active Martian Storm in Jezero Crater
Authors:	Lemmon, M. T.; Smith, M. D.; Viudez-Moreiras, D.; de la Torre-Juarez, M.; Vicente-Retortillo, A.; Munguira, A.; Sanchez-Lavega, A.; Hueso, R.; Martinez, G.; Chide, B.; Sullivan, R.; Toledo, D.; Tamppari, L.; Bertrand, T.; Bell, J. F.; Newman, C.; Baker, M.; Banfield, D.; Rodriguez-Manfredi, J. A.; Maki, J. N.; Apestigue, V.
Affiliation:	AA(Space Science Institute, Boulder, CO USA), AB(NASA Goddard Space Flight Center, Greenbelt, MD USA), AC(Centro de Astrobiologia (INTA-CSIC), Madrid, Spain), AD(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AE(Centro de Astrobiologia (INTA-CSIC), Madrid, Spain), AF(Física Aplicada, Escuela de Ingeniería de Bilbao, UPV/EHU, Bilbao, Spain), AG(Física Aplicada, Escuela de Ingeniería de Bilbao, UPV/EHU, Bilbao, Spain), AH(Física Aplicada, Escuela de Ingeniería de Bilbao, UPV/EHU, Bilbao, Spain), AI(Lunar and Planetary Institute, Houston, TX USA), AJ(Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM USA), AK(Cornell University, Ithaca, NY USA), AL(Instituto Nacional de Técnica Aerospacial, Madrid, Spain), AM(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AN(LESIA, Observatoire de Paris, Meudon, France), AO(Arizona State University, Tempe, AZ USA), AP(Aeolis Research, Chandler, AZ USA), AQ(Smithsonian National Air and Space Museum, Washington, DC USA), AR(Cornell University, Ithaca, NY USA), AS(Centro de Astrobiologia (INTA-CSIC), Madrid, Spain), AT(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AU(Instituto Nacional de Técnica Aerospacial, Madrid, Spain)
Journal:	Geophysical Research Letters, Volume 49, Issue 17, article id. e00126.
Publication Date:	Sep 2022
Origin:	American Geophysical Union (AGU)
Abstract Copyright:	2022. American Geophysical Union. All Rights Reserved.
DOI:	https://doi.org/10.1029/2022GL100126
Bibliographic Code:	2022GeoRL..4900126L
Abstract:	Rovers and landers on Mars have experienced local, regional, and planetary-scale dust storms. However, in situ documentation of active lifting within storms has remained elusive. Over 5-11 January 2022 (L<SUB>S</SUB> 153°-156°), a dust storm passed over the Perseverance rover site. Peak visible optical depth was ∼2, and visibility across the crater was briefly reduced. Pressure amplitudes and temperatures responded to the storm. Winds up to 20 m s<SUP>-1</SUP> rotated around the site before the wind sensor was damaged. The rover imaged 21 dust-lifting events—gusts and dust devils—in one 25-min period, and at least three events mobilized sediment near the rover. Rover tracks and drill cuttings were extensively modified, and debris was moved onto the rover deck. Migration of small ripples was seen, but there was no large-scale change in undisturbed areas. This work presents an overview of observations and initial results from the study of the storm.

Title:	The Aeolian Environment in Glen Torridon, Gale Crater, Mars
Authors:	Sullivan, R.; Baker, M.; Newman, C.; Turner, M.; Schieber, J.; Weitz, C.; Hallet, B.; Ellison, D.; Minitti, M.
Affiliation:	AA(CCAPS, Cornell University, Ithaca, NY USA), AB(Center for Earth & Planetary Studies, National Air & Space Museum, Smithsonian Institution, Washington, DC USA), AC(Aeolis Research, Pasadena, CA USA), AD(The Johns Hopkins University Morton K. Blaustein Department of Earth and Planetary Sciences, Baltimore, MD USA), AE(Department of Geological Sciences, Indiana University, Bloomington, IN USA), AF(Planetary Science Institute, Tucson, AZ USA), AG(University of Washington, Seattle, WA USA), AH(Jet Propulion Laboratory, Pasadena, CA USA), AI(Framework, Silver Spring, MD USA)
Journal:	Journal of Geophysical Research: Planets, Volume 127, Issue 8, article id. e07174.
Publication Date:	Aug 2022
Origin:	American Geophysical Union (AGU)
Keywords:	Mars, aeolian, Glen Torridon
Abstract Copyright:	2022. American Geophysical Union. All Rights Reserved.
DOI:	https://doi.org/10.1029/2021JE007174
Bibliographic Code:	2022JGRE..12707174S
Abstract:	The Mars Science Laboratory (MSL) rover spent a full martian year exploring the phyllosilicate-bearing Glen Torridon trough on the flank of Aeolis Mons in Gale crater, enabling in-depth assessment of aeolian processes. MSL encountered erosional and depositional features recording a long aeolian history. The trough has served as a long-term conduit for sand transport, probably involving many cycles of sand accumulation and deflation. Rock abrasion textures indicate sand-driving winds blowing W-SW (opposite of abrasion textures on the Greenheugh Pediment above the trough floor). Indurated megaripple surfaces with 2-5 mm grains contrast with seasonally active ripples having finer maximum grain sizes, indicating more vigorous saltation in the past. Active ripples display a broad continuum of wavelengths, as well as coarser grains at crests than troughs, consistent with origins as impact ripples. Orientations of a wind streak extending from a large ripple field, and sandy wind tails behind obstacles, indicate sand is driven W-SW in the current era, approximately along the trough axis. Erosion of drill tailings piles was strongly seasonal, enhanced during late spring and early summer (perihelion). Climate modeling suggests W-SW sand transport can be attributed to seasonal enhancement of nighttime regional winds entering Gale crater from the N, combined with local katabatic winds flowing down the slopes of Aeolis Mons. However, it is unclear whether sand transport at Glen Torridon is primarily from these wind components combining and acting simultaneously, or occurring in serial at different times of night; field evidence supports both possibilities.

Title:	Mars Surface Pressure Oscillations as Precursors of Large Dust Storms Reaching Gale
Authors:	Zurita-Zurita, S.; de la Torre Juárez, M.; Newman, C. E.; Viúdez-Moreiras, D.; Kahanpää, H. T.; Harri, A.-M.; Lemmon, M. T.; Pla-García, J.; Rodríguez-Manfredi, J. A.
Affiliation:	AA(Centro de Astrobiología (INTA-CSIC), Torrejón de Ardoz-Madrid, Spain), AB(Jet Propulsion Laboratory/California Institute of Technology, Pasadena, CA USA), AC(Aeolis Research, Chandler, AZ USA), AD(Centro de Astrobiología (INTA-CSIC), Torrejón de Ardoz-Madrid, Spain), AE(School of Electrical Engineering, Aalto University, Espoo, Finland), AF(Finnish Meteorological Institute, Helsinki, Finland), AG(Space Science Institute, College Station, TX USA), AH(Centro de Astrobiología (INTA-CSIC), Torrejón de Ardoz-Madrid, Spain), AI(Centro de Astrobiología (INTA-CSIC), Torrejón de Ardoz-Madrid, Spain)
Journal:	Journal of Geophysical Research: Planets, Volume 127, Issue 8, article id. e07005.
Publication Date:	Aug 2022
Origin:	American Geophysical Union (AGU)
Keywords:	Mars, dust storm precursors, surface pressure, planetary waves, emprical mode decomposition, singular spectrum analysis
Abstract Copyright:	2022. American Geophysical Union. All Rights Reserved.
DOI:	https://doi.org/10.1029/2021JE007005
Bibliographic Code:	2022JGRE..12707005Z
Abstract:	Modeling and observations have long demonstrated that Martian dust storms strongly interfere with global circulation patterns and change the diurnal and semidiurnal pressure variability as well as oscillations with periods greater than one sol associated with planetary waves. As of early 2022, five Mars years of pressure data have been collected by the Curiosity Rover in Gale crater with the Rover Environmental Monitoring Station (REMS). A combination of signal filtering techniques is used to search for pressure signatures that might warn large-scale dust storms reaching Gale. The analysis combines an exploration of changes in both baroclinic waves and thermal tides for the first time to our knowledge. Focusing on the periods preceding local opacity increases as detected by Curiosity's Mastcam observations, the pressure analysis shows changes in the coupling between the diurnal pressure tide and quasi-diurnal Kelvin wave, as well as in the temporal evolution of baroclinic waves that are harbingers of the larger dust storms. Changes in the phasing between Kelvin waves and diurnal tides are found to be precursors for the growth phase of periods Z (defined here as L<SUB>s</SUB> ∼ 120°-160°), A (L<SUB>s</SUB> ∼ 190°-240°), and C (L<SUB>s</SUB> ∼ 300°-335°) dust storms. Changes in multi-sol pressure oscillations also help predict the occurrence of A, B (L<SUB>s</SUB> ∼ 245°-295°), and C storms. The specific pressure oscillations preceding each storm period are likely to be signatures of the large-scale circulation patterns that enable the growth and propagation of the storm fronts.

Title:	Multi-year measurements of ripple and dune migration on Mars: Implications for the wind regime and sand transport
Authors:	Roback, Kevin P.; Runyon, Kirby; Newman, Claire; Avouac, Jean-Philippe
Affiliation:	AA(California Institute of Technology, Division of Geological and Planetary Sciences, Pasadena, CA, USA), AB(The Johns Hopkins University Applied Physics Laboratory, Laurel, MD, USA), AC(Aeolis Research, Tucson, AZ, USA), AD(California Institute of Technology, Division of Geological and Planetary Sciences, Pasadena, CA, USA)
Journal:	Icarus, Volume 380, article id. 114966.
Publication Date:	Jul 2022
Origin:	Elsevier BV
Keywords:	Mars, Aeolian geomorphology, Sand transport, Mars climate, Image correlation
Abstract Copyright:	(c) 2022 Elsevier Science B.V. All rights reserved.
DOI:	https://doi.org/10.1016/j.icarus.2022.114966
Bibliographic Code:	2022Icar..38014966R
Abstract:	Aeolian sand dunes are observed across the Martian surface. The arrival of the HiRISE camera on Mars Reconnaissance Orbiter at Mars in 2006 enabled detection of modern-day movement of dunes and ripples from orbit for the first time. Since 2006, HiRISE collected a long timeseries of repeat imagery at a few Martian dune fields. We analyze this timeseries of imagery at two of these dune fields, using COSI-Corr for image registration and correlation, to study the movement and dynamics of dunes and meter-scale ripples at the Nili Patera and Meroe Patera barchan dune fields. We present measurements of whole-dune translational sand fluxes extracted at both dune fields via manual tracking of dune crestlines and slipfaces in HiRISE images. We also present a multi-Mars year timeseries of ripple flux measurements. Ripple migration shows a consistent pattern of seasonal variation, with maxima in flux during northern-hemisphere autumn and winter at both dune fields. Ripple migration is also observed to decrease away from the upwind margins of dune fields. We compare our observations with predicted sand transport using winds output from the MarsWRF atmospheric circulation model and theories of sand motion. The model predicts half-hourly, mesoscale winds, from which we estimate the 1 Hz, local-scale winds by assuming a Weibull distribution of wind speed, with parameters chosen based on landed wind data. This approach uses remote sensing observations of bedform migration, and comparisons with model output, to place constraints on the wind regime. Our measurements of the seasonal pattern of sand flux variation agree, to first order, with predictions based on modeled wind speeds. Comparison of the magnitudes of predicted and observed sand fluxes is not feasible due to the high uncertainties in our calculated sand fluxes caused by uncertainties in input parameters, most importantly the assumed fluid threshold for sand transport. However, we note that model predictions fit our observed sand fluxes best when relatively low values of the fluid threshold shear velocity of ~0.6-0.8 m/s (or shear stresses of O(10<SUP>-3</SUP>) Pa) are assumed.

Title:	Earth-like thermal and dynamical coupling processes in the Martian climate system
Authors:	Wu, Zhaopeng; Li, Tao; Heavens, Nicholas G.; Newman, Claire E.; Richardson, Mark I.; Yang, Chengyun; Li, Jing; Cui, Jun
Affiliation:	AA(Planetary Environmental and Astrobiological Research Laboratory, School of Atmospheric Sciences, Sun Yat-Sen University, Zhuhai, Guangdong, 519082, China), AB(CAS Key Laboratory of Geospace Environment, School of Earth and Space Sciences, University of Science and Technology of China, Hefei, Anhui, China), AC(Department of Earth Science and Engineering, Imperial College, London, UK), AD(Aeolis Research, Chandler, AZ, USA), AE(Aeolis Research, Chandler, AZ, USA), AF(CAS Key Laboratory of Geospace Environment, School of Earth and Space Sciences, University of Science and Technology of China, Hefei, Anhui, China), AG(Planetary Environmental and Astrobiological Research Laboratory, School of Atmospheric Sciences, Sun Yat-Sen University, Zhuhai, Guangdong, 519082, China), AH(Planetary Environmental and Astrobiological Research Laboratory, School of Atmospheric Sciences, Sun Yat-Sen University, Zhuhai, Guangdong, 519082, China)
Journal:	Earth Science Reviews, Volume 229, article id. 104023.
Publication Date:	Jun 2022
Origin:	Elsevier BV
Abstract Copyright:	(c) 2022 Elsevier Science B.V. All rights reserved.
DOI:	https://doi.org/10.1016/j.earscirev.2022.104023
Bibliographic Code:	2022ESRv..22904023W
Abstract:	The burst of Mars exploration in the past two decades has significantly improved our knowledge of the Martian atmosphere. A variety of complementary, multiannual observational records have revealed Earth-like cycling of dust and water through the Mars system, as well as hints of dynamical coupling between the lower, middle, and upper atmosphere involving deep convection, planetary waves, thermal tides, and gravity waves that can be analogous to, but sometimes very different from, coupling processes in the Earth's atmosphere. This review focuses on several essential coupling processes on Mars involving the dust/water cycling and wave activity: (1) interaction between the dust cycle, water cycle and wave activity in the lower atmosphere; (2) the global meridional circulation and middle atmospheric polar warmings; and (3) vertical coupling throughout the atmosphere during dusty/non-dusty conditions. Most of these processes have been studied with state-of-the-art numerical models validated with recent observations. In addition, we summarize several newly proposed hypotheses that potentially impact our understanding of major issues in planetary science such as atmospheric coupling, water escape, or mesospheric cloud formation. We find many similarities between wave-induced couplings on Earth and Mars and analogies between the Earth's water cycle and Mars's dust cycle, which provide insights into comparative studies of these two planets.

Title:	Orbital and In-Situ Investigation of Periodic Bedrock Ridges in Glen Torridon, Gale Crater, Mars
Authors:	Stack, Kathryn M.; Dietrich, William E.; Lamb, Michael P.; Sullivan, Robert J.; Christian, John R.; Newman, Claire E.; O'Connell-Cooper, Catherine D.; Sneed, Jonathan W.; Day, Mackenzie; Baker, Mariah; Arvidson, Raymond E.; Fedo, Christopher M.; Khan, Sabrina; Williams, Rebecca M. E.; Bennett, Kristen A.; Bryk, Alexander B.; Cofield, Shannon; Edgar, Lauren A.; Fox, Valerie K.; Fraeman, Abigail A.; House, Christopher H.; Rubin, David M.; Sun, Vivian Z.; Van Beek, Jason K.
Affiliation:	AA(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AB(Department of Earth and Planetary Science, University of California, Berkeley, Berkeley, CA USA), AC(Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA USA), AD(Cornell Center for Astrophysics & Planetary Science, Cornell University, Ithaca, NY USA), AE(Department of Earth and Planetary Sciences, Washington University in St. Louis, St. Louis, MO USA), AF(Aeolis Research, Chandler, AZ USA), AG(Department of Earth Science, University of New Brunswick, Fredericton, NB Canada), AH(Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles, Los Angeles, CA USA), AI(Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles, Los Angeles, CA USA), AJ(Center for Earth & Planetary Studies, National Air & Space Museum, Smithsonian Institution, Washington, DC USA), AK(Department of Earth and Planetary Sciences, Washington University in St. Louis, St. Louis, MO USA), AL(Department of Earth and Planetary Sciences, University of Tennessee, Knoxville, Knoxville, TN USA), AM(Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA USA), AN(Planetary Science Institute, Tucson, AZ USA), AO(Astrogeology Science Center, U.S. Geological Survey, Flagstaff, AZ USA), AP(Department of Earth and Planetary Science, University of California, Berkeley, Berkeley, CA USA), AQ(U.S. Department of the Interior, Bureau of Ocean Energy Management, Washington, DC USA), AR(Astrogeology Science Center, U.S. Geological Survey, Flagstaff, AZ USA), AS(Earth and Environmental Sciences, University of Minnesota, Minneapolis, MN USA), AT(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AU(College of Earth and Mineral Sciences, Penn State University, University Park, PA USA), AV(Earth and Planetary Sciences, University of California, Santa Cruz, Santa Cruz, CA USA), AW(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AX(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA)
Journal:	Journal of Geophysical Research: Planets, Volume 127, Issue 6, article id. e07096.
Publication Date:	Jun 2022
Origin:	American Geophysical Union (AGU)
Keywords:	periodic bedrock ridges, Mars Science Laboratory, Gale crater, Glen Torridon, aeolian processes
Abstract Copyright:	2022 Jet Propulsion Laboratory. California Institute of Technology. Government sponsorship acknowledged.
DOI:	https://doi.org/10.1029/2021JE007096
Bibliographic Code:	2022JGRE..12707096S
Abstract:	Gale crater, the field site for NASA's Mars Science Laboratory Curiosity rover, contains a diverse and extensive record of aeolian deposition and erosion. This study focuses on a series of regularly spaced, curvilinear, and sometimes branching bedrock ridges that occur within the Glen Torridon region on the lower northwest flank of Aeolis Mons, the central mound within Gale crater. During Curiosity's exploration of Glen Torridon between sols ∼2300-3080, the rover drove through this field of ridges, providing the opportunity for in situ observation of these features. This study uses orbiter and rover data to characterize ridge morphology, spatial distribution, compositional and material properties, and association with other aeolian features in the area. Based on these observations, we find that the Glen Torridon ridges are consistent with an origin as wind-eroded bedrock ridges, carved during the exhumation of Mount Sharp. Erosional features like the Glen Torridon ridges observed elsewhere on Mars, termed periodic bedrock ridges (PBRs), have been interpreted to form transverse to the dominant wind direction. The size and morphology of the Glen Torridon PBRs are consistent with transverse formative winds, but the orientation of nearby aeolian bedforms and bedrock erosional features raise the possibility of PBR formation by a net northeasterly wind regime. Although several formation models for the Glen Torridon PBRs are still under consideration, and questions persist about the nature of PBR-forming paleowinds, the presence of PBRs at this site provides important constraints on the depositional and erosional history of Gale crater.

Title:	Variability in Titan's Mesospheric HCN and Temperature Structure as Observed by ALMA
Authors:	Thelen, Alexander E.; Nixon, Conor A.; Cosentino, Richard G.; Cordiner, Martin A.; Teanby, Nicholas A.; Newman, Claire E.; Irwin, Patrick G. J.; Charnley, Steven B.
Affiliation:	AA(Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA), AB(Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA), AC(Space Telescope Science Institute, Baltimore, MD 21218, USA), AD(Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA; Department of Physics, Catholic University of America, Washington, DC 20064, USA), AE(School of Earth Sciences, University of Bristol, Bristol BS8 1RJ, UK), AF(Aeolis Research, Chandler, AZ 85224, USA), AG(Atmospheric, Oceanic and Planetary Physics, Clarendon Laboratory, University of Oxford, Oxford OX1 3PU, UK), AH(Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA)
Journal:	The Planetary Science Journal, Volume 3, Issue 6, id.146, <NUMPAGES>13</NUMPAGES> pp.
Publication Date:	Jun 2022
Origin:	American Astronomical Society
Keywords:	Titan, Natural satellite atmospheres, Radiative transfer, Submillimeter astronomy, Planetary science, Solar system astronomy, Planetary atmospheres, Remote sensing, Astrochemistry, 2186, 2214, 1335, 1647, 1255, 1529, 1244, 2191, 75, Astrophysics - Earth and Planetary Astrophysics, Physics - Atmospheric and Oceanic Physics
DOI:	https://doi.org/10.3847/PSJ/ac7050
Bibliographic Code:	2022PSJ.....3..146T
Abstract:	The temperature structure of Titan's upper atmosphere exhibits large variability resulting from numerous spatially and temporally irregular external energy sources, seasonal changes, and the influence of molecular species produced via photochemistry. In particular, Titan's relatively abundant HCN is thought to provide substantial cooling to the upper atmosphere through rotational emission, balancing UV/EUV heating, and thermal conduction. Here we present the analysis of ALMA observations of Titan from 2012, 2014, 2015, and 2017, corresponding to planetocentric solar longitudes of ~34°-89°, including vertical HCN and temperature profiles retrieved from the lower mesosphere through the thermosphere (~350-1200 km; 3 × 10<SUP>-2</SUP>-2 × 10<SUP>-8</SUP> mbar). Throughout the atmosphere, temperature profiles differ by 10 to 30 K between observations approximately 1 Earth yr apart, particularly from 600 to 900 km. We find evidence for a large imbalance in Titan's upper atmospheric energy budget between 2014 and 2015, where the mesospheric thermal structure changes significantly and marks the transition between a mesopause located at ~600 km (2 × 10<SUP>-4</SUP> mbar) and ~800 km (3 × 10<SUP>-6</SUP> mbar). The retrieved HCN abundances vary dramatically during the 2012-2017 time period as well, showing close to 2 orders of magnitude difference in abundance at 1000 km. However, the change in HCN abundance does not appear to fully account for the variation in mesospheric temperatures over the L <SUB> S </SUB> ~ 34°-89° period. These measurements provide additional insight into the variability of Titan's mesospheric composition and thermal structure following its 2009 vernal equinox and motivate continued investigation of the origins of such rapid changes in Titan's atmosphere throughout its seasonal cycle.

Title:	The dynamic atmospheric and aeolian environment of Jezero crater, Mars
Authors:	Newman, Claire E.; Hueso, Ricardo; Lemmon, Mark T.; Munguira, Asier; Vicente-Retortillo, Álvaro; Apestigue, Víctor; Martínez, Germán M.; Toledo, Daniel; Sullivan, Rob; Herkenhoff, Ken E.; de la Torre Juárez, Manuel; Richardson, Mark I.; Stott, Alexander E.; Murdoch, Naomi; Sanchez-Lavega, Agustín; Wolff, Michael J.; Arruego, Ignacio; Sebastián, Eduardo; Navarro, Sara; Gómez-Elvira, Javier; Tamppari, Leslie; Viúdez-Moreiras, Daniel; Harri, Ari-Matti; Genzer, Maria; Hieta, Maria; Lorenz, Ralph D.; Conrad, Pan; Gómez, Felipe; McConnochie, Timothy H.; Mimoun, David; Tate, Christian; Bertrand, Tanguy; Bell, James F., III; Maki, Justin N.; Rodriguez-Manfredi, Jose Antonio; Wiens, Roger C.; Chide, Baptiste; Maurice, Sylvestre; Zorzano, Maria-Paz; Mora, Luis; Baker, Mariah M.; Banfield, Don; Pla-Garcia, Jorge; Beyssac, Olivier; Brown, Adrian; Clark, Ben; Lepinette, Alain; Montmessin, Franck; Fischer, Erik; Patel, Priyaben; del Río-Gaztelurrutia, Teresa; Fouchet, Thierry; Francis, Raymond; Guzewich, Scott D.
Journal:	Science Advances, vol. 8, issue 21, id. eabn3783.
Publication Date:	May 2022
Origin:	American Association for the Advancement of Science (AAAS)
DOI:	https://doi.org/10.1126/sciadv.abn3783
Bibliographic Code:	2022SciA....8N3783N
Abstract:	Despite the importance of sand and dust to Mars geomorphology, weather, and exploration, the processes that move sand and that raise dust to maintain Mars' ubiquitous dust haze and to produce dust storms have not been well quantified in situ, with missions lacking either the necessary sensors or a sufficiently active aeolian environment. Perseverance rover's novel environmental sensors and Jezero crater's dusty environment remedy this. In Perseverance's first 216 sols, four convective vortices raised dust locally, while, on average, four passed the rover daily, over 25% of which were significantly dusty ("dust devils"). More rarely, dust lifting by nonvortex wind gusts was produced by daytime convection cells advected over the crater by strong regional daytime upslope winds, which also control aeolian surface features. One such event covered 10 times more area than the largest dust devil, suggesting that dust devils and wind gusts could raise equal amounts of dust under nonstorm conditions. Perseverance sees huge aeolian activity due to strong daytime convection and slope flows, driving dust devils and wind gusts.

Title:	InSight Pressure Data Recalibration, and Its Application to the Study of Long-Term Pressure Changes on Mars
Authors:	Lange, L.; Forget, F.; Banfield, D.; Wolff, M.; Spiga, A.; Millour, E.; Viúdez-Moreiras, D.; Bierjon, A.; Piqueux, S.; Newman, C.; Pla-García, J.; Banerdt, W. B.
Affiliation:	AA(Laboratoire de Météorologie Dynamique,Institut Pierre-Simon Laplace (LMD/IPSL), Sorbonne Université, Centre National de la Recherche Scientifique (CNRS), École Polytechnique, École Normale Supérieure (ENS), Paris, France), AB(Laboratoire de Météorologie Dynamique,Institut Pierre-Simon Laplace (LMD/IPSL), Sorbonne Université, Centre National de la Recherche Scientifique (CNRS), École Polytechnique, École Normale Supérieure (ENS), Paris, France), AC(Cornell Center for Astrophysics and Planetary Science, Cornell University, Ithaca, NY USA), AD(Space Science Institute, Boulder, CO USA), AE(Laboratoire de Météorologie Dynamique,Institut Pierre-Simon Laplace (LMD/IPSL), Sorbonne Université, Centre National de la Recherche Scientifique (CNRS), École Polytechnique, École Normale Supérieure (ENS), Paris, France; Institut Universitaire de France, Paris, France), AF(Laboratoire de Météorologie Dynamique,Institut Pierre-Simon Laplace (LMD/IPSL), Sorbonne Université, Centre National de la Recherche Scientifique (CNRS), École Polytechnique, École Normale Supérieure (ENS), Paris, France), AG(Centro de Astrobiología (CSIC-INTA) and National Institute for Aerospace Technology (INTA), Madrid, Spain), AH(Laboratoire de Météorologie Dynamique,Institut Pierre-Simon Laplace (LMD/IPSL), Sorbonne Université, Centre National de la Recherche Scientifique (CNRS), École Polytechnique, École Normale Supérieure (ENS), Paris, France), AI(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AJ(Aeolis Research, Chandler, AZ USA), AK(Centro de Astrobiología (CSIC-INTA) and National Institute for Aerospace Technology (INTA), Madrid, Spain; Southwest Research Institute, Boulder, CO USA), AL(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA)
Journal:	Journal of Geophysical Research: Planets, Volume 127, Issue 5, article id. e07190.
Publication Date:	May 2022
Origin:	American Geophysical Union (AGU)
Keywords:	Mars, CO<SUB>2</SUB> ice, pressure, atmospheric mass, cap sublimation, Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract Copyright:	2022 The Authors.
DOI:	https://doi.org/10.1029/2022JE007190
Bibliographic Code:	2022JGRE..12707190L
Abstract:	Observations of the South Polar Residual Cap suggest a possible erosion of the cap, leading to an increase of the global mass of the atmosphere. We test this assumption by making the first comparison between Viking 1 and InSight surface pressure data, which were recorded 40 years apart. Such a comparison also allows us to determine changes in the dynamics of the seasonal ice caps between these two periods. To do so, we first had to recalibrate the InSight pressure data because of their unexpected sensitivity to the sensor temperature. Then, we had to design a procedure to compare distant pressure measurements. We propose two surface pressure interpolation methods at the local and global scale to do the comparison. The comparison of Viking and InSight seasonal surface pressure variations does not show changes larger than ±8 Pa in the CO<SUB>2</SUB> cycle. Such conclusions are supported by an analysis of Mars Science Laboratory (MSL) pressure data. Further comparisons with images of the south seasonal cap taken by the Viking 2 orbiter and MARCI camera do not display significant changes in the dynamics of this cap over a 40 year period. Only a possible larger extension of the North Cap after the global storm of MY 34 is observed, but the physical mechanisms behind this anomaly are not well determined. Finally, the first comparison of MSL and InSight pressure data suggests a pressure deficit at Gale crater during southern summer, possibly resulting from a large presence of dust suspended within the crater.

Title:	Changing spatial distribution of water flow charts major change in Mars's greenhouse effect
Authors:	Kite, Edwin S.; Mischna, Michael A.; Fan, Bowen; Morgan, Alexander M.; Wilson, Sharon A.; Richardson, Mark I.
Journal:	Science Advances, vol. 8, issue 21, id. eabo5894.
Publication Date:	May 2022
Origin:	American Association for the Advancement of Science (AAAS)
Keywords:	Astrophysics - Earth and Planetary Astrophysics, Physics - Atmospheric and Oceanic Physics, Physics - Geophysics
DOI:	https://doi.org/10.1126/sciadv.abo5894
Bibliographic Code:	2022SciA....8O5894K
Abstract:	Early Mars had rivers, but the cause of Mars's wet-to-dry transition remains unknown. Past climate on Mars can be probed using the spatial distribution of climate-sensitive landforms. We analyzed global databases of water-worked landforms and identified changes in the spatial distribution of rivers over time. These changes are simply explained by comparison to a simplified meltwater model driven by an ensemble of global climate model simulations, as the result of ≳10 K global cooling, from global average surface temperature T ̄ ≥ 268 K to T ̄ ~ 258 K, due to a weaker greenhouse effect. In other words, river-forming climates on early Mars were warm and wet first, and cold and wet later. Unexpectedly, analysis of the greenhouse effect within our ensemble of global climate model simulations suggests that this shift was primarily driven by waning non-CO 2 radiative forcing, and not changes in CO 2 radiative forcing. Climates on early Mars were warm and wet first, and cold and wet later, likely due to waning non-CO 2 radiative forcing.

Title:	In situ recording of Mars soundscape
Authors:	Maurice, S.; Chide, B.; Murdoch, N.; Lorenz, R. D.; Mimoun, D.; Wiens, R. C.; Stott, A.; Jacob, X.; Bertrand, T.; Montmessin, F.; Lanza, N. L.; Alvarez-Llamas, C.; Angel, S. M.; Aung, M.; Balaram, J.; Beyssac, O.; Cousin, A.; Delory, G.; Forni, O.; Fouchet, T.; Gasnault, O.; Grip, H.; Hecht, M.; Hoffman, J.; Laserna, J.; Lasue, J.; Maki, J.; McClean, J.; Meslin, P.-Y.; Le Mouélic, S.; Munguira, A.; Newman, C. E.; Rodríguez Manfredi, J. A.; Moros, J.; Ollila, A.; Pilleri, P.; Schröder, S.; de la Torre Juárez, M.; Tzanetos, T.; Stack, K. M.; Farley, K.; Williford, K.; SuperCam Team, Wiens, R. C.; Wiens, R. C.; Acosta-Maeda, T.; Acosta-Maeda, T.; Anderson, R. B.; Anderson, R. B.; Applin, D. M.; Arana, G.; Bassas-Portus, M.; Beal, R.; Beck, P.; Benzerara, K.; Bernard, S.; Bernardi, P.; Bernardi, P.; Bernardi, P.; Bosak, T.; Bousquet, B.; Brown, A.; Cadu, A.; Caïs, P.; Castro, K.; Castro, K.; Clavé, E.; Clegg, S. M.; Cloutis, E.; Connell, S.; Connell, S.; Debus, A.; Dehouck, E.; Delapp, D.; Donny, C.; Dorresoundiram, A.; Dromart, G.; Dubois, B.; Fabre, C.; Fau, A.; Fischer, W.; Fischer, W.; Fischer, W.; Francis, R.; Frydenvang, J.; Gabriel, T.; Gabriel, T.; Gibbons, E.; Gontijo, I.; Gontijo, I.; Johnson, J. R.; Kalucha, H.; Kelly, E.; Knutsen, E. W.; Lacombe, G.; Lacombe, G.; Lacombe, G.; Lacombe, G.; Le Mouélic, S.; Legett, C.; Leveille, R.; Lewin, E.; Lopez-Reyes, G.; Lopez-Reyes, G.; Lorigny, E.; Madariaga, J. M.; Madsen, M.; Madsen, S.; Mandon, L.; Mangold, N.; Mann, M.; Manrique, J.-A.; Martinez-Frias, J.; Mayhew, L. E.; McConnochie, T.; McLennan, S. M.; Melikechi, N.; Melikechi, N.; Meunier, F.; Meunier, F.; Montagnac, G.; Montagnac, G.; Montagnac, G.; Mousset, V.; Mousset, V.; Nelson, T.; Newell, R. T.; Newell, R. T.; Parot, Y.; Parot, Y.; Pilorget, C.; Pinet, P.; Pont, G.; Poulet, F.; Quantin-Nataf, C.; Quertier, B.; Rapin, W.; Reyes-Newell, A.; Robinson, S.; Rochas, L.; Royer, C.; Rull, F.; Sautter, V.; Sautter, V.; Sharma, S.; Shridar, V.; Sournac, A.; Sournac, A.; Toplis, M.; Torre-Fdez, I.; Turenne, N.; Turenne, N.; Udry, A.; Veneranda, M.; Venhaus, D.; Vogt, D.; Willis, P.
Affiliation:	AA(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France), AB(Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA), AC(Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France), AD(Space Exploration Sector, Johns Hopkins Applied Physics Laboratory, Laurel, MD, USA), AE(Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France), AF(Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA; Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN, USA), AG(Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France), AH(Institut de Mécanique des Fluides, Université de Toulouse 3 Paul Sabatier, INP, CNRS, Toulouse, France), AI(Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris, CNRS, Sorbonne Université, Université Paris Diderot, Meudon, France), AJ(Laboratoire Atmosphères, Milieux, Observations Spatiales, CNRS, Université Saint-Quentin-en-Yvelines, Sorbonne Université, Guyancourt, France), AK(Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA), AL(Universidad de Málaga, Málaga, Spain), AM(Department of Chemistry and Biochemistry, University of South Carolina, Columbia, SC, USA), AN(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA), AO(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA), AP(Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, CNRS, Sorbonne Université, MNHN, Paris, France), AQ(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France), AR(Heliospace Corporation, Berkeley, CA, USA), AS(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France), AT(Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris, CNRS, Sorbonne Université, Université Paris Diderot, Meudon, France), AU(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France), AV(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA), AW(Haystack Observatory, Massachusetts Institute of Technology, Westford, MA, USA), AX(Department of Aeronautics and Astronautics, Massachusetts Institute of Technology, Cambridge, MA, USA), AY(Universidad de Málaga, Málaga, Spain), AZ(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France), BA(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA), BB(Haystack Observatory, Massachusetts Institute of Technology, Westford, MA, USA), BC(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France), BD(Laboratoire de Planétologie et Géosciences, CNRS, Nantes Université, Université Angers, Nantes, France), BE(Escuela de Ingeniería de Bilbao, Universidad del País Vasco UPV/EHU, Bilbao, Spain), BF(Aeolis Corporation, Sierra Madre, CA, USA), BG(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), BH(Universidad de Málaga, Málaga, Spain), BI(Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA), BJ(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France), BK(Deutsches Zentrum für Luft- und Raumfahrt (DLR), Institute of Optical Sensor Systems, Berlin, Germany), BL(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA), BM(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA), BN(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA), BO(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA), BP(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA; Blue Marble Space Institute of Science, Seattle, WA, USA), BQ(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France; Department of Chemistry and Biochemistry, University of South Carolina, Columbia, SC, USA; Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA; Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, CNRS, Sorbonne Université, MNHN, Paris, France; Heliospace Corporation, Berkeley, CA, USA; Haystack Observatory, Massachusetts Institute of Technology, Westford, MA, USA; Department of Aeronautics and Astronautics, Massachusetts Institute of Technology, Cambridge, MA, USA; Laboratoire de Planétologie et Géosciences, CNRS, Nantes Université, Université Angers, Nantes, France; Escuela de Ingeniería de Bilbao, Universidad del País Vasco UPV/EHU, Bilbao, Spain; Aeolis Corporation, Sierra Madre, CA, USA; Centro de Astrobiología (INTA-CSIC), Madrid, Spain; Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA; Deutsches Zentrum für Luft- und Raumfahrt (DLR), Institute of Optical Sensor Systems, Berlin, Germany; Blue Marble Space Institute of Science, Seattle, WA, USA; University of Hawai`i at Mānoa, Mānoa, HI, USA; U.S. Geological Survey, Flagstaff, AZ, USA; University of Winnipeg, Winnipeg, Canada; University of the Basque Country UPV/EHU, Leioa, Bilbao, Spain; Institut de Planétologie et Astrophysique de Grenoble, CNRS, Université Grenoble Alpes, Grenoble, France; Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA; Centre Lasers Intenses et Applications, CNRS, CEA, Université de Bordeaux, Bordeaux, France; Plancius Research, Severna Park, MD, USA; Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France; Laboratoire d'Astrophysique de Bordeaux, CNRS, Université de Bordeaux, Bordeaux, France; Centre National d'Études Spatiales, Toulouse, France; Université de Lyon, UCBL, ENSL, UJM, CNRS, LGL-TPE, Villeurbanne, France; Groupe d'Instrumentation Scientifique, Observatoire Midi-Pyrénées, Toulouse, France; GeoRessources, CNRS, Université de Lorraine, Nancy, France; California Institute of Technology, Pasadena, CA, USA; University of Copenhagen, Copenhagen, Denmark; McGill University, Montreal, Canada; University of Valladolid, Valladolid, Spain; Agencia Estatal Consejo Superior de Investigaciones Científicas, Madrid, Spain; Space Exploration Sector, Johns Hopkins Applied Physics Laboratory, Laurel, MD, USA; Department of Geological Sciences, University of Colorado Boulder, Boulder, CO, USA; University of Maryland, College Park, MD, USA; State University of New York, Stony Brook, NY, USA; Department of Physics and Applied Physics, Kennedy College of Sciences, University of Massachusetts Lowell, Lowell, MA, USA; Institut d'Astrophysique Spatiale, CNRS, Université Paris-Saclay, Orsay, France; Institut Universitaire de France, Paris, France; University of Nevada, Las Vegas, Las Vegas, NV, USA; Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN, USA; Institut de Mécanique des Fluides, Université de Toulouse 3 Paul Sabatier, INP, CNRS, Toulouse, France; Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris, CNRS, Sorbonne Université, Université Paris Diderot, Meudon, France; Laboratoire Atmosphères, Milieux, Observations Spatiales, CNRS, Université Saint-Quentin-en-Yvelines, Sorbonne Université, Guyancourt, France; Universidad de Málaga, Málaga, Spain), BR(Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA), BS(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France; Department of Chemistry and Biochemistry, University of South Carolina, Columbia, SC, USA; Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA; Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, CNRS, Sorbonne Université, MNHN, Paris, France; Heliospace Corporation, Berkeley, CA, USA; Haystack Observatory, Massachusetts Institute of Technology, Westford, MA, USA; Department of Aeronautics and Astronautics, Massachusetts Institute of Technology, Cambridge, MA, USA; Laboratoire de Planétologie et Géosciences, CNRS, Nantes Université, Université Angers, Nantes, France; Escuela de Ingeniería de Bilbao, Universidad del País Vasco UPV/EHU, Bilbao, Spain; Aeolis Corporation, Sierra Madre, CA, USA; Centro de Astrobiología (INTA-CSIC), Madrid, Spain; Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA; Deutsches Zentrum für Luft- und Raumfahrt (DLR), Institute of Optical Sensor Systems, Berlin, Germany; Blue Marble Space Institute of Science, Seattle, WA, USA; University of Hawai`i at Mānoa, Mānoa, HI, USA; U.S. Geological Survey, Flagstaff, AZ, USA; University of Winnipeg, Winnipeg, Canada; University of the Basque Country UPV/EHU, Leioa, Bilbao, Spain; Institut de Planétologie et Astrophysique de Grenoble, CNRS, Université Grenoble Alpes, Grenoble, France; Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA; Centre Lasers Intenses et Applications, CNRS, CEA, Université de Bordeaux, Bordeaux, France; Plancius Research, Severna Park, MD, USA; Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France; Laboratoire d'Astrophysique de Bordeaux, CNRS, Université de Bordeaux, Bordeaux, France; Centre National d'Études Spatiales, Toulouse, France; Université de Lyon, UCBL, ENSL, UJM, CNRS, LGL-TPE, Villeurbanne, France; Groupe d'Instrumentation Scientifique, Observatoire Midi-Pyrénées, Toulouse, France; GeoRessources, CNRS, Université de Lorraine, Nancy, France; California Institute of Technology, Pasadena, CA, USA; University of Copenhagen, Copenhagen, Denmark; McGill University, Montreal, Canada; University of Valladolid, Valladolid, Spain; Agencia Estatal Consejo Superior de Investigaciones Científicas, Madrid, Spain; Space Exploration Sector, Johns Hopkins Applied Physics Laboratory, Laurel, MD, USA; Department of Geological Sciences, University of Colorado Boulder, Boulder, CO, USA; University of Maryland, College Park, MD, USA; State University of New York, Stony Brook, NY, USA; Department of Physics and Applied Physics, Kennedy College of Sciences, University of Massachusetts Lowell, Lowell, MA, USA; Institut d'Astrophysique Spatiale, CNRS, Université Paris-Saclay, Orsay, France; Institut Universitaire de France, Paris, France; University of Nevada, Las Vegas, Las Vegas, NV, USA; Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN, USA; Institut de Mécanique des Fluides, Université de Toulouse 3 Paul Sabatier, INP, CNRS, Toulouse, France; Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris, CNRS, Sorbonne Université, Université Paris Diderot, Meudon, France; Laboratoire Atmosphères, Milieux, Observations Spatiales, CNRS, Université Saint-Quentin-en-Yvelines, Sorbonne Université, Guyancourt, France; Universidad de Málaga, Málaga, Spain), BT(University of Hawai`i at Mānoa, Mānoa, HI, USA), BU(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France; Department of Chemistry and Biochemistry, University of South Carolina, Columbia, SC, USA; Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA; Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, CNRS, Sorbonne Université, MNHN, Paris, France; Heliospace Corporation, Berkeley, CA, USA; Haystack Observatory, Massachusetts Institute of Technology, Westford, MA, USA; Department of Aeronautics and Astronautics, Massachusetts Institute of Technology, Cambridge, MA, USA; Laboratoire de Planétologie et Géosciences, CNRS, Nantes Université, Université Angers, Nantes, France; Escuela de Ingeniería de Bilbao, Universidad del País Vasco UPV/EHU, Bilbao, Spain; Aeolis Corporation, Sierra Madre, CA, USA; Centro de Astrobiología (INTA-CSIC), Madrid, Spain; Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA; Deutsches Zentrum für Luft- und Raumfahrt (DLR), Institute of Optical Sensor Systems, Berlin, Germany; Blue Marble Space Institute of Science, Seattle, WA, USA; University of Hawai`i at Mānoa, Mānoa, HI, USA; U.S. Geological Survey, Flagstaff, AZ, USA; University of Winnipeg, Winnipeg, Canada; University of the Basque Country UPV/EHU, Leioa, Bilbao, Spain; Institut de Planétologie et Astrophysique de Grenoble, CNRS, Université Grenoble Alpes, Grenoble, France; Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA; Centre Lasers Intenses et Applications, CNRS, CEA, Université de Bordeaux, Bordeaux, France; Plancius Research, Severna Park, MD, USA; Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France; Laboratoire d'Astrophysique de Bordeaux, CNRS, Université de Bordeaux, Bordeaux, France; Centre National d'Études Spatiales, Toulouse, France; Université de Lyon, UCBL, ENSL, UJM, CNRS, LGL-TPE, Villeurbanne, France; Groupe d'Instrumentation Scientifique, Observatoire Midi-Pyrénées, Toulouse, France; GeoRessources, CNRS, Université de Lorraine, Nancy, France; California Institute of Technology, Pasadena, CA, USA; University of Copenhagen, Copenhagen, Denmark; McGill University, Montreal, Canada; University of Valladolid, Valladolid, Spain; Agencia Estatal Consejo Superior de Investigaciones Científicas, Madrid, Spain; Space Exploration Sector, Johns Hopkins Applied Physics Laboratory, Laurel, MD, USA; Department of Geological Sciences, University of Colorado Boulder, Boulder, CO, USA; University of Maryland, College Park, MD, USA; State University of New York, Stony Brook, NY, USA; Department of Physics and Applied Physics, Kennedy College of Sciences, University of Massachusetts Lowell, Lowell, MA, USA; Institut d'Astrophysique Spatiale, CNRS, Université Paris-Saclay, Orsay, France; Institut Universitaire de France, Paris, France; University of Nevada, Las Vegas, Las Vegas, NV, USA; Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN, USA; Institut de Mécanique des Fluides, Université de Toulouse 3 Paul Sabatier, INP, CNRS, Toulouse, France; Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris, CNRS, Sorbonne Université, Université Paris Diderot, Meudon, France; Laboratoire Atmosphères, Milieux, Observations Spatiales, CNRS, Université Saint-Quentin-en-Yvelines, Sorbonne Université, Guyancourt, France; Universidad de Málaga, Málaga, Spain), BV(U.S. Geological Survey, Flagstaff, AZ, USA), BW(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France; Department of Chemistry and Biochemistry, University of South Carolina, Columbia, SC, USA; Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA; Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, CNRS, Sorbonne Université, MNHN, Paris, France; Heliospace Corporation, Berkeley, CA, USA; Haystack Observatory, Massachusetts Institute of Technology, Westford, MA, USA; Department of Aeronautics and Astronautics, Massachusetts Institute of Technology, Cambridge, MA, USA; Laboratoire de Planétologie et Géosciences, CNRS, Nantes Université, Université Angers, Nantes, France; Escuela de Ingeniería de Bilbao, Universidad del País Vasco UPV/EHU, Bilbao, Spain; Aeolis Corporation, Sierra Madre, CA, USA; Centro de Astrobiología (INTA-CSIC), Madrid, Spain; Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA; Deutsches Zentrum für Luft- und Raumfahrt (DLR), Institute of Optical Sensor Systems, Berlin, Germany; Blue Marble Space Institute of Science, Seattle, WA, USA; University of Hawai`i at Mānoa, Mānoa, HI, USA; U.S. Geological Survey, Flagstaff, AZ, USA; University of Winnipeg, Winnipeg, Canada; University of the Basque Country UPV/EHU, Leioa, Bilbao, Spain; Institut de Planétologie et Astrophysique de Grenoble, CNRS, Université Grenoble Alpes, Grenoble, France; Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA; Centre Lasers Intenses et Applications, CNRS, CEA, Université de Bordeaux, Bordeaux, France; Plancius Research, Severna Park, MD, USA; Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France; Laboratoire d'Astrophysique de Bordeaux, CNRS, Université de Bordeaux, Bordeaux, France; Centre National d'Études Spatiales, Toulouse, France; Université de Lyon, UCBL, ENSL, UJM, CNRS, LGL-TPE, Villeurbanne, France; Groupe d'Instrumentation Scientifique, Observatoire Midi-Pyrénées, Toulouse, France; GeoRessources, CNRS, Université de Lorraine, Nancy, France; California Institute of Technology, Pasadena, CA, USA; University of Copenhagen, Copenhagen, Denmark; McGill University, Montreal, Canada; University of Valladolid, Valladolid, Spain; Agencia Estatal Consejo Superior de Investigaciones Científicas, Madrid, Spain; Space Exploration Sector, Johns Hopkins Applied Physics Laboratory, Laurel, MD, USA; Department of Geological Sciences, University of Colorado Boulder, Boulder, CO, USA; University of Maryland, College Park, MD, USA; State University of New York, Stony Brook, NY, USA; Department of Physics and Applied Physics, Kennedy College of Sciences, University of Massachusetts Lowell, Lowell, MA, USA; Institut d'Astrophysique Spatiale, CNRS, Université Paris-Saclay, Orsay, France; Institut Universitaire de France, Paris, France; University of Nevada, Las Vegas, Las Vegas, NV, USA; Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN, USA; Institut de Mécanique des Fluides, Université de Toulouse 3 Paul Sabatier, INP, CNRS, Toulouse, France; Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris, CNRS, Sorbonne Université, Université Paris Diderot, Meudon, France; Laboratoire Atmosphères, Milieux, Observations Spatiales, CNRS, Université Saint-Quentin-en-Yvelines, Sorbonne Université, Guyancourt, France; Universidad de Málaga, Málaga, Spain), BX(University of Winnipeg, Winnipeg, Canada), BY(University of the Basque Country UPV/EHU, Leioa, Bilbao, Spain), BZ(Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France), CA(Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA), CB(Institut de Planétologie et Astrophysique de Grenoble, CNRS, Université Grenoble Alpes, Grenoble, France), CC(Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, CNRS, Sorbonne Université, MNHN, Paris, France), CD(Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, CNRS, Sorbonne Université, MNHN, Paris, France), CE(Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris, CNRS, Sorbonne Université, Université Paris Diderot, Meudon, France), CF(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France; Department of Chemistry and Biochemistry, University of South Carolina, Columbia, SC, USA; Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA; Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, CNRS, Sorbonne Université, MNHN, Paris, France; Heliospace Corporation, Berkeley, CA, USA; Haystack Observatory, Massachusetts Institute of Technology, Westford, MA, USA; Department of Aeronautics and Astronautics, Massachusetts Institute of Technology, Cambridge, MA, USA; Laboratoire de Planétologie et Géosciences, CNRS, Nantes Université, Université Angers, Nantes, France; Escuela de Ingeniería de Bilbao, Universidad del País Vasco UPV/EHU, Bilbao, Spain; Aeolis Corporation, Sierra Madre, CA, USA; Centro de Astrobiología (INTA-CSIC), Madrid, Spain; Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA; Deutsches Zentrum für Luft- und Raumfahrt (DLR), Institute of Optical Sensor Systems, Berlin, Germany; Blue Marble Space Institute of Science, Seattle, WA, USA; University of Hawai`i at Mānoa, Mānoa, HI, USA; U.S. Geological Survey, Flagstaff, AZ, USA; University of Winnipeg, Winnipeg, Canada; University of the Basque Country UPV/EHU, Leioa, Bilbao, Spain; Institut de Planétologie et Astrophysique de Grenoble, CNRS, Université Grenoble Alpes, Grenoble, France; Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA; Centre Lasers Intenses et Applications, CNRS, CEA, Université de Bordeaux, Bordeaux, France; Plancius Research, Severna Park, MD, USA; Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France; Laboratoire d'Astrophysique de Bordeaux, CNRS, Université de Bordeaux, Bordeaux, France; Centre National d'Études Spatiales, Toulouse, France; Université de Lyon, UCBL, ENSL, UJM, CNRS, LGL-TPE, Villeurbanne, France; Groupe d'Instrumentation Scientifique, Observatoire Midi-Pyrénées, Toulouse, France; GeoRessources, CNRS, Université de Lorraine, Nancy, France; California Institute of Technology, Pasadena, CA, USA; University of Copenhagen, Copenhagen, Denmark; McGill University, Montreal, Canada; University of Valladolid, Valladolid, Spain; Agencia Estatal Consejo Superior de Investigaciones Científicas, Madrid, Spain; Space Exploration Sector, Johns Hopkins Applied Physics Laboratory, Laurel, MD, USA; Department of Geological Sciences, University of Colorado Boulder, Boulder, CO, USA; University of Maryland, College Park, MD, USA; State University of New York, Stony Brook, NY, USA; Department of Physics and Applied Physics, Kennedy College of Sciences, University of Massachusetts Lowell, Lowell, MA, USA; Institut d'Astrophysique Spatiale, CNRS, Université Paris-Saclay, Orsay, France; Institut Universitaire de France, Paris, France; University of Nevada, Las Vegas, Las Vegas, NV, USA; Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN, USA; Institut de Mécanique des Fluides, Université de Toulouse 3 Paul Sabatier, INP, CNRS, Toulouse, France; Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris, CNRS, Sorbonne Université, Université Paris Diderot, Meudon, France; Laboratoire Atmosphères, Milieux, Observations Spatiales, CNRS, Université Saint-Quentin-en-Yvelines, Sorbonne Université, Guyancourt, France; Universidad de Málaga, Málaga, Spain), CG(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France; Department of Chemistry and Biochemistry, University of South Carolina, Columbia, SC, USA; Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA; Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, CNRS, Sorbonne Université, MNHN, Paris, France; Heliospace Corporation, Berkeley, CA, USA; Haystack Observatory, Massachusetts Institute of Technology, Westford, MA, USA; Department of Aeronautics and Astronautics, Massachusetts Institute of Technology, Cambridge, MA, USA; Laboratoire de Planétologie et Géosciences, CNRS, Nantes Université, Université Angers, Nantes, France; Escuela de Ingeniería de Bilbao, Universidad del País Vasco UPV/EHU, Bilbao, Spain; Aeolis Corporation, Sierra Madre, CA, USA; Centro de Astrobiología (INTA-CSIC), Madrid, Spain; Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA; Deutsches Zentrum für Luft- und Raumfahrt (DLR), Institute of Optical Sensor Systems, Berlin, Germany; Blue Marble Space Institute of Science, Seattle, WA, USA; University of Hawai`i at Mānoa, Mānoa, HI, USA; U.S. Geological Survey, Flagstaff, AZ, USA; University of Winnipeg, Winnipeg, Canada; University of the Basque Country UPV/EHU, Leioa, Bilbao, Spain; Institut de Planétologie et Astrophysique de Grenoble, CNRS, Université Grenoble Alpes, Grenoble, France; Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA; Centre Lasers Intenses et Applications, CNRS, CEA, Université de Bordeaux, Bordeaux, France; Plancius Research, Severna Park, MD, USA; Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France; Laboratoire d'Astrophysique de Bordeaux, CNRS, Université de Bordeaux, Bordeaux, France; Centre National d'Études Spatiales, Toulouse, France; Université de Lyon, UCBL, ENSL, UJM, CNRS, LGL-TPE, Villeurbanne, France; Groupe d'Instrumentation Scientifique, Observatoire Midi-Pyrénées, Toulouse, France; GeoRessources, CNRS, Université de Lorraine, Nancy, France; California Institute of Technology, Pasadena, CA, USA; University of Copenhagen, Copenhagen, Denmark; McGill University, Montreal, Canada; University of Valladolid, Valladolid, Spain; Agencia Estatal Consejo Superior de Investigaciones Científicas, Madrid, Spain; Space Exploration Sector, Johns Hopkins Applied Physics Laboratory, Laurel, MD, USA; Department of Geological Sciences, University of Colorado Boulder, Boulder, CO, USA; University of Maryland, College Park, MD, USA; State University of New York, Stony Brook, NY, USA; Department of Physics and Applied Physics, Kennedy College of Sciences, University of Massachusetts Lowell, Lowell, MA, USA; Institut d'Astrophysique Spatiale, CNRS, Université Paris-Saclay, Orsay, France; Institut Universitaire de France, Paris, France; University of Nevada, Las Vegas, Las Vegas, NV, USA; Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN, USA; Institut de Mécanique des Fluides, Université de Toulouse 3 Paul Sabatier, INP, CNRS, Toulouse, France; Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris, CNRS, Sorbonne Université, Université Paris Diderot, Meudon, France; Laboratoire Atmosphères, Milieux, Observations Spatiales, CNRS, Université Saint-Quentin-en-Yvelines, Sorbonne Université, Guyancourt, France; Universidad de Málaga, Málaga, Spain), CH(Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA), CI(Centre Lasers Intenses et Applications, CNRS, CEA, Université de Bordeaux, Bordeaux, France), CJ(Plancius Research, Severna Park, MD, USA), CK(Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France), CL(Laboratoire d'Astrophysique de Bordeaux, CNRS, Université de Bordeaux, Bordeaux, France), CM(University of the Basque Country UPV/EHU, Leioa, Bilbao, Spain), CN(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France; Department of Chemistry and Biochemistry, University of South Carolina, Columbia, SC, USA; Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA; Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, CNRS, Sorbonne Université, MNHN, Paris, France; Heliospace Corporation, Berkeley, CA, USA; Haystack Observatory, Massachusetts Institute of Technology, Westford, MA, USA; Department of Aeronautics and Astronautics, Massachusetts Institute of Technology, Cambridge, MA, USA; Laboratoire de Planétologie et Géosciences, CNRS, Nantes Université, Université Angers, Nantes, France; Escuela de Ingeniería de Bilbao, Universidad del País Vasco UPV/EHU, Bilbao, Spain; Aeolis Corporation, Sierra Madre, CA, USA; Centro de Astrobiología (INTA-CSIC), Madrid, Spain; Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA; Deutsches Zentrum für Luft- und Raumfahrt (DLR), Institute of Optical Sensor Systems, Berlin, Germany; Blue Marble Space Institute of Science, Seattle, WA, USA; University of Hawai`i at Mānoa, Mānoa, HI, USA; U.S. Geological Survey, Flagstaff, AZ, USA; University of Winnipeg, Winnipeg, Canada; University of the Basque Country UPV/EHU, Leioa, Bilbao, Spain; Institut de Planétologie et Astrophysique de Grenoble, CNRS, Université Grenoble Alpes, Grenoble, France; Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA; Centre Lasers Intenses et Applications, CNRS, CEA, Université de Bordeaux, Bordeaux, France; Plancius Research, Severna Park, MD, USA; Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France; Laboratoire d'Astrophysique de Bordeaux, CNRS, Université de Bordeaux, Bordeaux, France; Centre National d'Études Spatiales, Toulouse, France; Université de Lyon, UCBL, ENSL, UJM, CNRS, LGL-TPE, Villeurbanne, France; Groupe d'Instrumentation Scientifique, Observatoire Midi-Pyrénées, Toulouse, France; GeoRessources, CNRS, Université de Lorraine, Nancy, France; California Institute of Technology, Pasadena, CA, USA; University of Copenhagen, Copenhagen, Denmark; McGill University, Montreal, Canada; University of Valladolid, Valladolid, Spain; Agencia Estatal Consejo Superior de Investigaciones Científicas, Madrid, Spain; Space Exploration Sector, Johns Hopkins Applied Physics Laboratory, Laurel, MD, USA; Department of Geological Sciences, University of Colorado Boulder, Boulder, CO, USA; University of Maryland, College Park, MD, USA; State University of New York, Stony Brook, NY, USA; Department of Physics and Applied Physics, Kennedy College of Sciences, University of Massachusetts Lowell, Lowell, MA, USA; Institut d'Astrophysique Spatiale, CNRS, Université Paris-Saclay, Orsay, France; Institut Universitaire de France, Paris, France; University of Nevada, Las Vegas, Las Vegas, NV, USA; Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN, USA; Institut de Mécanique des Fluides, Université de Toulouse 3 Paul Sabatier, INP, CNRS, Toulouse, France; Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris, CNRS, Sorbonne Université, Université Paris Diderot, Meudon, France; Laboratoire Atmosphères, Milieux, Observations Spatiales, CNRS, Université Saint-Quentin-en-Yvelines, Sorbonne Université, Guyancourt, France; Universidad de Málaga, Málaga, Spain), CO(Centre Lasers Intenses et Applications, CNRS, CEA, Université de Bordeaux, Bordeaux, France), CP(Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA), CQ(University of Winnipeg, Winnipeg, Canada), CR(University of Winnipeg, Winnipeg, Canada), CS(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France; Department of Chemistry and Biochemistry, University of South Carolina, Columbia, SC, USA; Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA; Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, CNRS, Sorbonne Université, MNHN, Paris, France; Heliospace Corporation, Berkeley, CA, USA; Haystack Observatory, Massachusetts Institute of Technology, Westford, MA, USA; Department of Aeronautics and Astronautics, Massachusetts Institute of Technology, Cambridge, MA, USA; Laboratoire de Planétologie et Géosciences, CNRS, Nantes Université, Université Angers, Nantes, France; Escuela de Ingeniería de Bilbao, Universidad del País Vasco UPV/EHU, Bilbao, Spain; Aeolis Corporation, Sierra Madre, CA, USA; Centro de Astrobiología (INTA-CSIC), Madrid, Spain; Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA; Deutsches Zentrum für Luft- und Raumfahrt (DLR), Institute of Optical Sensor Systems, Berlin, Germany; Blue Marble Space Institute of Science, Seattle, WA, USA; University of Hawai`i at Mānoa, Mānoa, HI, USA; U.S. Geological Survey, Flagstaff, AZ, USA; University of Winnipeg, Winnipeg, Canada; University of the Basque Country UPV/EHU, Leioa, Bilbao, Spain; Institut de Planétologie et Astrophysique de Grenoble, CNRS, Université Grenoble Alpes, Grenoble, France; Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA; Centre Lasers Intenses et Applications, CNRS, CEA, Université de Bordeaux, Bordeaux, France; Plancius Research, Severna Park, MD, USA; Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France; Laboratoire d'Astrophysique de Bordeaux, CNRS, Université de Bordeaux, Bordeaux, France; Centre National d'Études Spatiales, Toulouse, France; Université de Lyon, UCBL, ENSL, UJM, CNRS, LGL-TPE, Villeurbanne, France; Groupe d'Instrumentation Scientifique, Observatoire Midi-Pyrénées, Toulouse, France; GeoRessources, CNRS, Université de Lorraine, Nancy, France; California Institute of Technology, Pasadena, CA, USA; University of Copenhagen, Copenhagen, Denmark; McGill University, Montreal, Canada; University of Valladolid, Valladolid, Spain; Agencia Estatal Consejo Superior de Investigaciones Científicas, Madrid, Spain; Space Exploration Sector, Johns Hopkins Applied Physics Laboratory, Laurel, MD, USA; Department of Geological Sciences, University of Colorado Boulder, Boulder, CO, USA; University of Maryland, College Park, MD, USA; State University of New York, Stony Brook, NY, USA; Department of Physics and Applied Physics, Kennedy College of Sciences, University of Massachusetts Lowell, Lowell, MA, USA; Institut d'Astrophysique Spatiale, CNRS, Université Paris-Saclay, Orsay, France; Institut Universitaire de France, Paris, France; University of Nevada, Las Vegas, Las Vegas, NV, USA; Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN, USA; Institut de Mécanique des Fluides, Université de Toulouse 3 Paul Sabatier, INP, CNRS, Toulouse, France; Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris, CNRS, Sorbonne Université, Université Paris Diderot, Meudon, France; Laboratoire Atmosphères, Milieux, Observations Spatiales, CNRS, Université Saint-Quentin-en-Yvelines, Sorbonne Université, Guyancourt, France; Universidad de Málaga, Málaga, Spain), CT(Centre National d'Études Spatiales, Toulouse, France), CU(Université de Lyon, UCBL, ENSL, UJM, CNRS, LGL-TPE, Villeurbanne, France), CV(Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA), CW(Centre National d'Études Spatiales, Toulouse, France), CX(Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris, CNRS, Sorbonne Université, Université Paris Diderot, Meudon, France), CY(Université de Lyon, UCBL, ENSL, UJM, CNRS, LGL-TPE, Villeurbanne, France), CZ(Groupe d'Instrumentation Scientifique, Observatoire Midi-Pyrénées, Toulouse, France), DA(GeoRessources, CNRS, Université de Lorraine, Nancy, France), DB(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France), DC(California Institute of Technology, Pasadena, CA, USA), DD(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France; Department of Chemistry and Biochemistry, University of South Carolina, Columbia, SC, USA; Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA; Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, CNRS, Sorbonne Université, MNHN, Paris, France; Heliospace Corporation, Berkeley, CA, USA; Haystack Observatory, Massachusetts Institute of Technology, Westford, MA, USA; Department of Aeronautics and Astronautics, Massachusetts Institute of Technology, Cambridge, MA, USA; Laboratoire de Planétologie et Géosciences, CNRS, Nantes Université, Université Angers, Nantes, France; Escuela de Ingeniería de Bilbao, Universidad del País Vasco UPV/EHU, Bilbao, Spain; Aeolis Corporation, Sierra Madre, CA, USA; Centro de Astrobiología (INTA-CSIC), Madrid, Spain; Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA; Deutsches Zentrum für Luft- und Raumfahrt (DLR), Institute of Optical Sensor Systems, Berlin, Germany; Blue Marble Space Institute of Science, Seattle, WA, USA; University of Hawai`i at Mānoa, Mānoa, HI, USA; U.S. Geological Survey, Flagstaff, AZ, USA; University of Winnipeg, Winnipeg, Canada; University of the Basque Country UPV/EHU, Leioa, Bilbao, Spain; Institut de Planétologie et Astrophysique de Grenoble, CNRS, Université Grenoble Alpes, Grenoble, France; Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA; Centre Lasers Intenses et Applications, CNRS, CEA, Université de Bordeaux, Bordeaux, France; Plancius Research, Severna Park, MD, USA; Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France; Laboratoire d'Astrophysique de Bordeaux, CNRS, Université de Bordeaux, Bordeaux, France; Centre National d'Études Spatiales, Toulouse, France; Université de Lyon, UCBL, ENSL, UJM, CNRS, LGL-TPE, Villeurbanne, France; Groupe d'Instrumentation Scientifique, Observatoire Midi-Pyrénées, Toulouse, France; GeoRessources, CNRS, Université de Lorraine, Nancy, France; California Institute of Technology, Pasadena, CA, USA; University of Copenhagen, Copenhagen, Denmark; McGill University, Montreal, Canada; University of Valladolid, Valladolid, Spain; Agencia Estatal Consejo Superior de Investigaciones Científicas, Madrid, Spain; Space Exploration Sector, Johns Hopkins Applied Physics Laboratory, Laurel, MD, USA; Department of Geological Sciences, University of Colorado Boulder, Boulder, CO, USA; University of Maryland, College Park, MD, USA; State University of New York, Stony Brook, NY, USA; Department of Physics and Applied Physics, Kennedy College of Sciences, University of Massachusetts Lowell, Lowell, MA, USA; Institut d'Astrophysique Spatiale, CNRS, Université Paris-Saclay, Orsay, France; Institut Universitaire de France, Paris, France; University of Nevada, Las Vegas, Las Vegas, NV, USA; Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN, USA; Institut de Mécanique des Fluides, Université de Toulouse 3 Paul Sabatier, INP, CNRS, Toulouse, France; Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris, CNRS, Sorbonne Université, Université Paris Diderot, Meudon, France; Laboratoire Atmosphères, Milieux, Observations Spatiales, CNRS, Université Saint-Quentin-en-Yvelines, Sorbonne Université, Guyancourt, France; Universidad de Málaga, Málaga, Spain), DE(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France; Department of Chemistry and Biochemistry, University of South Carolina, Columbia, SC, USA; Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA; Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, CNRS, Sorbonne Université, MNHN, Paris, France; Heliospace Corporation, Berkeley, CA, USA; Haystack Observatory, Massachusetts Institute of Technology, Westford, MA, USA; Department of Aeronautics and Astronautics, Massachusetts Institute of Technology, Cambridge, MA, USA; Laboratoire de Planétologie et Géosciences, CNRS, Nantes Université, Université Angers, Nantes, France; Escuela de Ingeniería de Bilbao, Universidad del País Vasco UPV/EHU, Bilbao, Spain; Aeolis Corporation, Sierra Madre, CA, USA; Centro de Astrobiología (INTA-CSIC), Madrid, Spain; Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA; Deutsches Zentrum für Luft- und Raumfahrt (DLR), Institute of Optical Sensor Systems, Berlin, Germany; Blue Marble Space Institute of Science, Seattle, WA, USA; University of Hawai`i at Mānoa, Mānoa, HI, USA; U.S. Geological Survey, Flagstaff, AZ, USA; University of Winnipeg, Winnipeg, Canada; University of the Basque Country UPV/EHU, Leioa, Bilbao, Spain; Institut de Planétologie et Astrophysique de Grenoble, CNRS, Université Grenoble Alpes, Grenoble, France; Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA; Centre Lasers Intenses et Applications, CNRS, CEA, Université de Bordeaux, Bordeaux, France; Plancius Research, Severna Park, MD, USA; Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France; Laboratoire d'Astrophysique de Bordeaux, CNRS, Université de Bordeaux, Bordeaux, France; Centre National d'Études Spatiales, Toulouse, France; Université de Lyon, UCBL, ENSL, UJM, CNRS, LGL-TPE, Villeurbanne, France; Groupe d'Instrumentation Scientifique, Observatoire Midi-Pyrénées, Toulouse, France; GeoRessources, CNRS, Université de Lorraine, Nancy, France; California Institute of Technology, Pasadena, CA, USA; University of Copenhagen, Copenhagen, Denmark; McGill University, Montreal, Canada; University of Valladolid, Valladolid, Spain; Agencia Estatal Consejo Superior de Investigaciones Científicas, Madrid, Spain; Space Exploration Sector, Johns Hopkins Applied Physics Laboratory, Laurel, MD, USA; Department of Geological Sciences, University of Colorado Boulder, Boulder, CO, USA; University of Maryland, College Park, MD, USA; State University of New York, Stony Brook, NY, USA; Department of Physics and Applied Physics, Kennedy College of Sciences, University of Massachusetts Lowell, Lowell, MA, USA; Institut d'Astrophysique Spatiale, CNRS, Université Paris-Saclay, Orsay, France; Institut Universitaire de France, Paris, France; University of Nevada, Las Vegas, Las Vegas, NV, USA; Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN, USA; Institut de Mécanique des Fluides, Université de Toulouse 3 Paul Sabatier, INP, CNRS, Toulouse, France; Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris, CNRS, Sorbonne Université, Université Paris Diderot, Meudon, France; Laboratoire Atmosphères, Milieux, Observations Spatiales, CNRS, Université Saint-Quentin-en-Yvelines, Sorbonne Université, Guyancourt, France; Universidad de Málaga, Málaga, Spain), DF(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA), DG(University of Copenhagen, Copenhagen, Denmark), DH(U.S. Geological Survey, Flagstaff, AZ, USA), DI(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France; Department of Chemistry and Biochemistry, University of South Carolina, Columbia, SC, USA; Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA; Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, CNRS, Sorbonne Université, MNHN, Paris, France; Heliospace Corporation, Berkeley, CA, USA; Haystack Observatory, Massachusetts Institute of Technology, Westford, MA, USA; Department of Aeronautics and Astronautics, Massachusetts Institute of Technology, Cambridge, MA, USA; Laboratoire de Planétologie et Géosciences, CNRS, Nantes Université, Université Angers, Nantes, France; Escuela de Ingeniería de Bilbao, Universidad del País Vasco UPV/EHU, Bilbao, Spain; Aeolis Corporation, Sierra Madre, CA, USA; Centro de Astrobiología (INTA-CSIC), Madrid, Spain; Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA; Deutsches Zentrum für Luft- und Raumfahrt (DLR), Institute of Optical Sensor Systems, Berlin, Germany; Blue Marble Space Institute of Science, Seattle, WA, USA; University of Hawai`i at Mānoa, Mānoa, HI, USA; U.S. Geological Survey, Flagstaff, AZ, USA; University of Winnipeg, Winnipeg, Canada; University of the Basque Country UPV/EHU, Leioa, Bilbao, Spain; Institut de Planétologie et Astrophysique de Grenoble, CNRS, Université Grenoble Alpes, Grenoble, France; Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA; Centre Lasers Intenses et Applications, CNRS, CEA, Université de Bordeaux, Bordeaux, France; Plancius Research, Severna Park, MD, USA; Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France; Laboratoire d'Astrophysique de Bordeaux, CNRS, Université de Bordeaux, Bordeaux, France; Centre National d'Études Spatiales, Toulouse, France; Université de Lyon, UCBL, ENSL, UJM, CNRS, LGL-TPE, Villeurbanne, France; Groupe d'Instrumentation Scientifique, Observatoire Midi-Pyrénées, Toulouse, France; GeoRessources, CNRS, Université de Lorraine, Nancy, France; California Institute of Technology, Pasadena, CA, USA; University of Copenhagen, Copenhagen, Denmark; McGill University, Montreal, Canada; University of Valladolid, Valladolid, Spain; Agencia Estatal Consejo Superior de Investigaciones Científicas, Madrid, Spain; Space Exploration Sector, Johns Hopkins Applied Physics Laboratory, Laurel, MD, USA; Department of Geological Sciences, University of Colorado Boulder, Boulder, CO, USA; University of Maryland, College Park, MD, USA; State University of New York, Stony Brook, NY, USA; Department of Physics and Applied Physics, Kennedy College of Sciences, University of Massachusetts Lowell, Lowell, MA, USA; Institut d'Astrophysique Spatiale, CNRS, Université Paris-Saclay, Orsay, France; Institut Universitaire de France, Paris, France; University of Nevada, Las Vegas, Las Vegas, NV, USA; Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN, USA; Institut de Mécanique des Fluides, Université de Toulouse 3 Paul Sabatier, INP, CNRS, Toulouse, France; Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris, CNRS, Sorbonne Université, Université Paris Diderot, Meudon, France; Laboratoire Atmosphères, Milieux, Observations Spatiales, CNRS, Université Saint-Quentin-en-Yvelines, Sorbonne Université, Guyancourt, France; Universidad de Málaga, Málaga, Spain), DJ(McGill University, Montreal, Canada), DK(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA), DL(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France; Department of Chemistry and Biochemistry, University of South Carolina, Columbia, SC, USA; Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA; Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, CNRS, Sorbonne Université, MNHN, Paris, France; Heliospace Corporation, Berkeley, CA, USA; Haystack Observatory, Massachusetts Institute of Technology, Westford, MA, USA; Department of Aeronautics and Astronautics, Massachusetts Institute of Technology, Cambridge, MA, USA; Laboratoire de Planétologie et Géosciences, CNRS, Nantes Université, Université Angers, Nantes, France; Escuela de Ingeniería de Bilbao, Universidad del País Vasco UPV/EHU, Bilbao, Spain; Aeolis Corporation, Sierra Madre, CA, USA; Centro de Astrobiología (INTA-CSIC), Madrid, Spain; Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA; Deutsches Zentrum für Luft- und Raumfahrt (DLR), Institute of Optical Sensor Systems, Berlin, Germany; Blue Marble Space Institute of Science, Seattle, WA, USA; University of Hawai`i at Mānoa, Mānoa, HI, USA; U.S. Geological Survey, Flagstaff, AZ, USA; University of Winnipeg, Winnipeg, Canada; University of the Basque Country UPV/EHU, Leioa, Bilbao, Spain; Institut de Planétologie et Astrophysique de Grenoble, CNRS, Université Grenoble Alpes, Grenoble, France; Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA; Centre Lasers Intenses et Applications, CNRS, CEA, Université de Bordeaux, Bordeaux, France; Plancius Research, Severna Park, MD, USA; Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France; Laboratoire d'Astrophysique de Bordeaux, CNRS, Université de Bordeaux, Bordeaux, France; Centre National d'Études Spatiales, Toulouse, France; Université de Lyon, UCBL, ENSL, UJM, CNRS, LGL-TPE, Villeurbanne, France; Groupe d'Instrumentation Scientifique, Observatoire Midi-Pyrénées, Toulouse, France; GeoRessources, CNRS, Université de Lorraine, Nancy, France; California Institute of Technology, Pasadena, CA, USA; University of Copenhagen, Copenhagen, Denmark; McGill University, Montreal, Canada; University of Valladolid, Valladolid, Spain; Agencia Estatal Consejo Superior de Investigaciones Científicas, Madrid, Spain; Space Exploration Sector, Johns Hopkins Applied Physics Laboratory, Laurel, MD, USA; Department of Geological Sciences, University of Colorado Boulder, Boulder, CO, USA; University of Maryland, College Park, MD, USA; State University of New York, Stony Brook, NY, USA; Department of Physics and Applied Physics, Kennedy College of Sciences, University of Massachusetts Lowell, Lowell, MA, USA; Institut d'Astrophysique Spatiale, CNRS, Université Paris-Saclay, Orsay, France; Institut Universitaire de France, Paris, France; University of Nevada, Las Vegas, Las Vegas, NV, USA; Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN, USA; Institut de Mécanique des Fluides, Université de Toulouse 3 Paul Sabatier, INP, CNRS, Toulouse, France; Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris, CNRS, Sorbonne Université, Université Paris Diderot, Meudon, France; Laboratoire Atmosphères, Milieux, Observations Spatiales, CNRS, Université Saint-Quentin-en-Yvelines, Sorbonne Université, Guyancourt, France; Universidad de Málaga, Málaga, Spain), DM(Space Exploration Sector, Johns Hopkins Applied Physics Laboratory, Laurel, MD, USA), DN(California Institute of Technology, Pasadena, CA, USA), DO(University of Hawai`i at Mānoa, Mānoa, HI, USA), DP(Laboratoire Atmosphères, Milieux, Observations Spatiales, CNRS, Université Saint-Quentin-en-Yvelines, Sorbonne Université, Guyancourt, France), DQ(Laboratoire Atmosphères, Milieux, Observations Spatiales, CNRS, Université Saint-Quentin-en-Yvelines, Sorbonne Université, Guyancourt, France), DR(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France; Department of Chemistry and Biochemistry, University of South Carolina, Columbia, SC, USA; Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA; Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, CNRS, Sorbonne Université, MNHN, Paris, France; Heliospace Corporation, Berkeley, CA, USA; Haystack Observatory, Massachusetts Institute of Technology, Westford, MA, USA; Department of Aeronautics and Astronautics, Massachusetts Institute of Technology, Cambridge, MA, USA; Laboratoire de Planétologie et Géosciences, CNRS, Nantes Université, Université Angers, Nantes, France; Escuela de Ingeniería de Bilbao, Universidad del País Vasco UPV/EHU, Bilbao, Spain; Aeolis Corporation, Sierra Madre, CA, USA; Centro de Astrobiología (INTA-CSIC), Madrid, Spain; Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA; Deutsches Zentrum für Luft- und Raumfahrt (DLR), Institute of Optical Sensor Systems, Berlin, Germany; Blue Marble Space Institute of Science, Seattle, WA, USA; University of Hawai`i at Mānoa, Mānoa, HI, USA; U.S. Geological Survey, Flagstaff, AZ, USA; University of Winnipeg, Winnipeg, Canada; University of the Basque Country UPV/EHU, Leioa, Bilbao, Spain; Institut de Planétologie et Astrophysique de Grenoble, CNRS, Université Grenoble Alpes, Grenoble, France; Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA; Centre Lasers Intenses et Applications, CNRS, CEA, Université de Bordeaux, Bordeaux, France; Plancius Research, Severna Park, MD, USA; Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France; Laboratoire d'Astrophysique de Bordeaux, CNRS, Université de Bordeaux, Bordeaux, France; Centre National d'Études Spatiales, Toulouse, France; Université de Lyon, UCBL, ENSL, UJM, CNRS, LGL-TPE, Villeurbanne, France; Groupe d'Instrumentation Scientifique, Observatoire Midi-Pyrénées, Toulouse, France; GeoRessources, CNRS, Université de Lorraine, Nancy, France; California Institute of Technology, Pasadena, CA, USA; University of Copenhagen, Copenhagen, Denmark; McGill University, Montreal, Canada; University of Valladolid, Valladolid, Spain; Agencia Estatal Consejo Superior de Investigaciones Científicas, Madrid, Spain; Space Exploration Sector, Johns Hopkins Applied Physics Laboratory, Laurel, MD, USA; Department of Geological Sciences, University of Colorado Boulder, Boulder, CO, USA; University of Maryland, College Park, MD, USA; State University of New York, Stony Brook, NY, USA; Department of Physics and Applied Physics, Kennedy College of Sciences, University of Massachusetts Lowell, Lowell, MA, USA; Institut d'Astrophysique Spatiale, CNRS, Université Paris-Saclay, Orsay, France; Institut Universitaire de France, Paris, France; University of Nevada, Las Vegas, Las Vegas, NV, USA; Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN, USA; Institut de Mécanique des Fluides, Université de Toulouse 3 Paul Sabatier, INP, CNRS, Toulouse, France; Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris, CNRS, Sorbonne Université, Université Paris Diderot, Meudon, France; Laboratoire Atmosphères, Milieux, Observations Spatiales, CNRS, Université Saint-Quentin-en-Yvelines, Sorbonne Université, Guyancourt, France; Universidad de Málaga, Málaga, Spain), DS(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France; Department of Chemistry and Biochemistry, University of South Carolina, Columbia, SC, USA; Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA; Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, CNRS, Sorbonne Université, MNHN, Paris, France; Heliospace Corporation, Berkeley, CA, USA; Haystack Observatory, Massachusetts Institute of Technology, Westford, MA, USA; Department of Aeronautics and Astronautics, Massachusetts Institute of Technology, Cambridge, MA, USA; Laboratoire de Planétologie et Géosciences, CNRS, Nantes Université, Université Angers, Nantes, France; Escuela de Ingeniería de Bilbao, Universidad del País Vasco UPV/EHU, Bilbao, Spain; Aeolis Corporation, Sierra Madre, CA, USA; Centro de Astrobiología (INTA-CSIC), Madrid, Spain; Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA; Deutsches Zentrum für Luft- und Raumfahrt (DLR), Institute of Optical Sensor Systems, Berlin, Germany; Blue Marble Space Institute of Science, Seattle, WA, USA; University of Hawai`i at Mānoa, Mānoa, HI, USA; U.S. Geological Survey, Flagstaff, AZ, USA; University of Winnipeg, Winnipeg, Canada; University of the Basque Country UPV/EHU, Leioa, Bilbao, Spain; Institut de Planétologie et Astrophysique de Grenoble, CNRS, Université Grenoble Alpes, Grenoble, France; Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA; Centre Lasers Intenses et Applications, CNRS, CEA, Université de Bordeaux, Bordeaux, France; Plancius Research, Severna Park, MD, USA; Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France; Laboratoire d'Astrophysique de Bordeaux, CNRS, Université de Bordeaux, Bordeaux, France; Centre National d'Études Spatiales, Toulouse, France; Université de Lyon, UCBL, ENSL, UJM, CNRS, LGL-TPE, Villeurbanne, France; Groupe d'Instrumentation Scientifique, Observatoire Midi-Pyrénées, Toulouse, France; GeoRessources, CNRS, Université de Lorraine, Nancy, France; California Institute of Technology, Pasadena, CA, USA; University of Copenhagen, Copenhagen, Denmark; McGill University, Montreal, Canada; University of Valladolid, Valladolid, Spain; Agencia Estatal Consejo Superior de Investigaciones Científicas, Madrid, Spain; Space Exploration Sector, Johns Hopkins Applied Physics Laboratory, Laurel, MD, USA; Department of Geological Sciences, University of Colorado Boulder, Boulder, CO, USA; University of Maryland, College Park, MD, USA; State University of New York, Stony Brook, NY, USA; Department of Physics and Applied Physics, Kennedy College of Sciences, University of Massachusetts Lowell, Lowell, MA, USA; Institut d'Astrophysique Spatiale, CNRS, Université Paris-Saclay, Orsay, France; Institut Universitaire de France, Paris, France; University of Nevada, Las Vegas, Las Vegas, NV, USA; Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN, USA; Institut de Mécanique des Fluides, Université de Toulouse 3 Paul Sabatier, INP, CNRS, Toulouse, France; Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris, CNRS, Sorbonne Université, Université Paris Diderot, Meudon, France; Laboratoire Atmosphères, Milieux, Observations Spatiales, CNRS, Université Saint-Quentin-en-Yvelines, Sorbonne Université, Guyancourt, France; Universidad de Málaga, Málaga, Spain), DT(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France; Department of Chemistry and Biochemistry, University of South Carolina, Columbia, SC, USA; Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA; Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, CNRS, Sorbonne Université, MNHN, Paris, France; Heliospace Corporation, Berkeley, CA, USA; Haystack Observatory, Massachusetts Institute of Technology, Westford, MA, USA; Department of Aeronautics and Astronautics, Massachusetts Institute of Technology, Cambridge, MA, USA; Laboratoire de Planétologie et Géosciences, CNRS, Nantes Université, Université Angers, Nantes, France; Escuela de Ingeniería de Bilbao, Universidad del País Vasco UPV/EHU, Bilbao, Spain; Aeolis Corporation, Sierra Madre, CA, USA; Centro de Astrobiología (INTA-CSIC), Madrid, Spain; Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA; Deutsches Zentrum für Luft- und Raumfahrt (DLR), Institute of Optical Sensor Systems, Berlin, Germany; Blue Marble Space Institute of Science, Seattle, WA, USA; University of Hawai`i at Mānoa, Mānoa, HI, USA; U.S. Geological Survey, Flagstaff, AZ, USA; University of Winnipeg, Winnipeg, Canada; University of the Basque Country UPV/EHU, Leioa, Bilbao, Spain; Institut de Planétologie et Astrophysique de Grenoble, CNRS, Université Grenoble Alpes, Grenoble, France; Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA; Centre Lasers Intenses et Applications, CNRS, CEA, Université de Bordeaux, Bordeaux, France; Plancius Research, Severna Park, MD, USA; Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France; Laboratoire d'Astrophysique de Bordeaux, CNRS, Université de Bordeaux, Bordeaux, France; Centre National d'Études Spatiales, Toulouse, France; Université de Lyon, UCBL, ENSL, UJM, CNRS, LGL-TPE, Villeurbanne, France; Groupe d'Instrumentation Scientifique, Observatoire Midi-Pyrénées, Toulouse, France; GeoRessources, CNRS, Université de Lorraine, Nancy, France; California Institute of Technology, Pasadena, CA, USA; University of Copenhagen, Copenhagen, Denmark; McGill University, Montreal, Canada; University of Valladolid, Valladolid, Spain; Agencia Estatal Consejo Superior de Investigaciones Científicas, Madrid, Spain; Space Exploration Sector, Johns Hopkins Applied Physics Laboratory, Laurel, MD, USA; Department of Geological Sciences, University of Colorado Boulder, Boulder, CO, USA; University of Maryland, College Park, MD, USA; State University of New York, Stony Brook, NY, USA; Department of Physics and Applied Physics, Kennedy College of Sciences, University of Massachusetts Lowell, Lowell, MA, USA; Institut d'Astrophysique Spatiale, CNRS, Université Paris-Saclay, Orsay, France; Institut Universitaire de France, Paris, France; University of Nevada, Las Vegas, Las Vegas, NV, USA; Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN, USA; Institut de Mécanique des Fluides, Université de Toulouse 3 Paul Sabatier, INP, CNRS, Toulouse, France; Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris, CNRS, Sorbonne Université, Université Paris Diderot, Meudon, France; Laboratoire Atmosphères, Milieux, Observations Spatiales, CNRS, Université Saint-Quentin-en-Yvelines, Sorbonne Université, Guyancourt, France; Universidad de Málaga, Málaga, Spain), DU(Laboratoire de Planétologie et Géosciences, CNRS, Nantes Université, Université Angers, Nantes, France), DV(Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA), DW(McGill University, Montreal, Canada), DX(Institut de Planétologie et Astrophysique de Grenoble, CNRS, Université Grenoble Alpes, Grenoble, France), DY(University of Valladolid, Valladolid, Spain), DZ(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France; Department of Chemistry and Biochemistry, University of South Carolina, Columbia, SC, USA; Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA; Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, CNRS, Sorbonne Université, MNHN, Paris, France; Heliospace Corporation, Berkeley, CA, USA; Haystack Observatory, Massachusetts Institute of Technology, Westford, MA, USA; Department of Aeronautics and Astronautics, Massachusetts Institute of Technology, Cambridge, MA, USA; Laboratoire de Planétologie et Géosciences, CNRS, Nantes Université, Université Angers, Nantes, France; Escuela de Ingeniería de Bilbao, Universidad del País Vasco UPV/EHU, Bilbao, Spain; Aeolis Corporation, Sierra Madre, CA, USA; Centro de Astrobiología (INTA-CSIC), Madrid, Spain; Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA; Deutsches Zentrum für Luft- und Raumfahrt (DLR), Institute of Optical Sensor Systems, Berlin, Germany; Blue Marble Space Institute of Science, Seattle, WA, USA; University of Hawai`i at Mānoa, Mānoa, HI, USA; U.S. Geological Survey, Flagstaff, AZ, USA; University of Winnipeg, Winnipeg, Canada; University of the Basque Country UPV/EHU, Leioa, Bilbao, Spain; Institut de Planétologie et Astrophysique de Grenoble, CNRS, Université Grenoble Alpes, Grenoble, France; Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA; Centre Lasers Intenses et Applications, CNRS, CEA, Université de Bordeaux, Bordeaux, France; Plancius Research, Severna Park, MD, USA; Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France; Laboratoire d'Astrophysique de Bordeaux, CNRS, Université de Bordeaux, Bordeaux, France; Centre National d'Études Spatiales, Toulouse, France; Université de Lyon, UCBL, ENSL, UJM, CNRS, LGL-TPE, Villeurbanne, France; Groupe d'Instrumentation Scientifique, Observatoire Midi-Pyrénées, Toulouse, France; GeoRessources, CNRS, Université de Lorraine, Nancy, France; California Institute of Technology, Pasadena, CA, USA; University of Copenhagen, Copenhagen, Denmark; McGill University, Montreal, Canada; University of Valladolid, Valladolid, Spain; Agencia Estatal Consejo Superior de Investigaciones Científicas, Madrid, Spain; Space Exploration Sector, Johns Hopkins Applied Physics Laboratory, Laurel, MD, USA; Department of Geological Sciences, University of Colorado Boulder, Boulder, CO, USA; University of Maryland, College Park, MD, USA; State University of New York, Stony Brook, NY, USA; Department of Physics and Applied Physics, Kennedy College of Sciences, University of Massachusetts Lowell, Lowell, MA, USA; Institut d'Astrophysique Spatiale, CNRS, Université Paris-Saclay, Orsay, France; Institut Universitaire de France, Paris, France; University of Nevada, Las Vegas, Las Vegas, NV, USA; Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN, USA; Institut de Mécanique des Fluides, Université de Toulouse 3 Paul Sabatier, INP, CNRS, Toulouse, France; Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris, CNRS, Sorbonne Université, Université Paris Diderot, Meudon, France; Laboratoire Atmosphères, Milieux, Observations Spatiales, CNRS, Université Saint-Quentin-en-Yvelines, Sorbonne Université, Guyancourt, France; Universidad de Málaga, Málaga, Spain), EA(Centre National d'Études Spatiales, Toulouse, France), EB(University of the Basque Country UPV/EHU, Leioa, Bilbao, Spain), EC(University of Copenhagen, Copenhagen, Denmark), ED(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA), EE(Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris, CNRS, Sorbonne Université, Université Paris Diderot, Meudon, France), EF(Laboratoire de Planétologie et Géosciences, CNRS, Nantes Université, Université Angers, Nantes, France), EG(Centre National d'Études Spatiales, Toulouse, France), EH(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France; University of Valladolid, Valladolid, Spain), EI(Agencia Estatal Consejo Superior de Investigaciones Científicas, Madrid, Spain), EJ(Department of Geological Sciences, University of Colorado Boulder, Boulder, CO, USA), EK(University of Maryland, College Park, MD, USA), EL(State University of New York, Stony Brook, NY, USA), EM(Department of Physics and Applied Physics, Kennedy College of Sciences, University of Massachusetts Lowell, Lowell, MA, USA), EN(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France; Department of Chemistry and Biochemistry, University of South Carolina, Columbia, SC, USA; Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA; Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, CNRS, Sorbonne Université, MNHN, Paris, France; Heliospace Corporation, Berkeley, CA, USA; Haystack Observatory, Massachusetts Institute of Technology, Westford, MA, USA; Department of Aeronautics and Astronautics, Massachusetts Institute of Technology, Cambridge, MA, USA; Laboratoire de Planétologie et Géosciences, CNRS, Nantes Université, Université Angers, Nantes, France; Escuela de Ingeniería de Bilbao, Universidad del País Vasco UPV/EHU, Bilbao, Spain; Aeolis Corporation, Sierra Madre, CA, USA; Centro de Astrobiología (INTA-CSIC), Madrid, Spain; Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA; Deutsches Zentrum für Luft- und Raumfahrt (DLR), Institute of Optical Sensor Systems, Berlin, Germany; Blue Marble Space Institute of Science, Seattle, WA, USA; University of Hawai`i at Mānoa, Mānoa, HI, USA; U.S. Geological Survey, Flagstaff, AZ, USA; University of Winnipeg, Winnipeg, Canada; University of the Basque Country UPV/EHU, Leioa, Bilbao, Spain; Institut de Planétologie et Astrophysique de Grenoble, CNRS, Université Grenoble Alpes, Grenoble, France; Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA; Centre Lasers Intenses et Applications, CNRS, CEA, Université de Bordeaux, Bordeaux, France; Plancius Research, Severna Park, MD, USA; Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France; Laboratoire d'Astrophysique de Bordeaux, CNRS, Université de Bordeaux, Bordeaux, France; Centre National d'Études Spatiales, Toulouse, France; Université de Lyon, UCBL, ENSL, UJM, CNRS, LGL-TPE, Villeurbanne, France; Groupe d'Instrumentation Scientifique, Observatoire Midi-Pyrénées, Toulouse, France; GeoRessources, CNRS, Université de Lorraine, Nancy, France; California Institute of Technology, Pasadena, CA, USA; University of Copenhagen, Copenhagen, Denmark; McGill University, Montreal, Canada; University of Valladolid, Valladolid, Spain; Agencia Estatal Consejo Superior de Investigaciones Científicas, Madrid, Spain; Space Exploration Sector, Johns Hopkins Applied Physics Laboratory, Laurel, MD, USA; Department of Geological Sciences, University of Colorado Boulder, Boulder, CO, USA; University of Maryland, College Park, MD, USA; State University of New York, Stony Brook, NY, USA; Department of Physics and Applied Physics, Kennedy College of Sciences, University of Massachusetts Lowell, Lowell, MA, USA; Institut d'Astrophysique Spatiale, CNRS, Université Paris-Saclay, Orsay, France; Institut Universitaire de France, Paris, France; University of Nevada, Las Vegas, Las Vegas, NV, USA; Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN, USA; Institut de Mécanique des Fluides, Université de Toulouse 3 Paul Sabatier, INP, CNRS, Toulouse, France; Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris, CNRS, Sorbonne Université, Université Paris Diderot, Meudon, France; Laboratoire Atmosphères, Milieux, Observations Spatiales, CNRS, Université Saint-Quentin-en-Yvelines, Sorbonne Université, Guyancourt, France; Universidad de Málaga, Málaga, Spain), EO(Centre National d'Études Spatiales, Toulouse, France), EP(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France; Department of Chemistry and Biochemistry, University of South Carolina, Columbia, SC, USA; Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA; Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, CNRS, Sorbonne Université, MNHN, Paris, France; Heliospace Corporation, Berkeley, CA, USA; Haystack Observatory, Massachusetts Institute of Technology, Westford, MA, USA; Department of Aeronautics and Astronautics, Massachusetts Institute of Technology, Cambridge, MA, USA; Laboratoire de Planétologie et Géosciences, CNRS, Nantes Université, Université Angers, Nantes, France; Escuela de Ingeniería de Bilbao, Universidad del País Vasco UPV/EHU, Bilbao, Spain; Aeolis Corporation, Sierra Madre, CA, USA; Centro de Astrobiología (INTA-CSIC), Madrid, Spain; Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA; Deutsches Zentrum für Luft- und Raumfahrt (DLR), Institute of Optical Sensor Systems, Berlin, Germany; Blue Marble Space Institute of Science, Seattle, WA, USA; University of Hawai`i at Mānoa, Mānoa, HI, USA; U.S. Geological Survey, Flagstaff, AZ, USA; University of Winnipeg, Winnipeg, Canada; University of the Basque Country UPV/EHU, Leioa, Bilbao, Spain; Institut de Planétologie et Astrophysique de Grenoble, CNRS, Université Grenoble Alpes, Grenoble, France; Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA; Centre Lasers Intenses et Applications, CNRS, CEA, Université de Bordeaux, Bordeaux, France; Plancius Research, Severna Park, MD, USA; Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France; Laboratoire d'Astrophysique de Bordeaux, CNRS, Université de Bordeaux, Bordeaux, France; Centre National d'Études Spatiales, Toulouse, France; Université de Lyon, UCBL, ENSL, UJM, CNRS, LGL-TPE, Villeurbanne, France; Groupe d'Instrumentation Scientifique, Observatoire Midi-Pyrénées, Toulouse, France; GeoRessources, CNRS, Université de Lorraine, Nancy, France; California Institute of Technology, Pasadena, CA, USA; University of Copenhagen, Copenhagen, Denmark; McGill University, Montreal, Canada; University of Valladolid, Valladolid, Spain; Agencia Estatal Consejo Superior de Investigaciones Científicas, Madrid, Spain; Space Exploration Sector, Johns Hopkins Applied Physics Laboratory, Laurel, MD, USA; Department of Geological Sciences, University of Colorado Boulder, Boulder, CO, USA; University of Maryland, College Park, MD, USA; State University of New York, Stony Brook, NY, USA; Department of Physics and Applied Physics, Kennedy College of Sciences, University of Massachusetts Lowell, Lowell, MA, USA; Institut d'Astrophysique Spatiale, CNRS, Université Paris-Saclay, Orsay, France; Institut Universitaire de France, Paris, France; University of Nevada, Las Vegas, Las Vegas, NV, USA; Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN, USA; Institut de Mécanique des Fluides, Université de Toulouse 3 Paul Sabatier, INP, CNRS, Toulouse, France; Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris, CNRS, Sorbonne Université, Université Paris Diderot, Meudon, France; Laboratoire Atmosphères, Milieux, Observations Spatiales, CNRS, Université Saint-Quentin-en-Yvelines, Sorbonne Université, Guyancourt, France; Universidad de Málaga, Málaga, Spain), EQ(Université de Lyon, UCBL, ENSL, UJM, CNRS, LGL-TPE, Villeurbanne, France), ER(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France; Department of Chemistry and Biochemistry, University of South Carolina, Columbia, SC, USA; Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA; Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, CNRS, Sorbonne Université, MNHN, Paris, France; Heliospace Corporation, Berkeley, CA, USA; Haystack Observatory, Massachusetts Institute of Technology, Westford, MA, USA; Department of Aeronautics and Astronautics, Massachusetts Institute of Technology, Cambridge, MA, USA; Laboratoire de Planétologie et Géosciences, CNRS, Nantes Université, Université Angers, Nantes, France; Escuela de Ingeniería de Bilbao, Universidad del País Vasco UPV/EHU, Bilbao, Spain; Aeolis Corporation, Sierra Madre, CA, USA; Centro de Astrobiología (INTA-CSIC), Madrid, Spain; Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA; Deutsches Zentrum für Luft- und Raumfahrt (DLR), Institute of Optical Sensor Systems, Berlin, Germany; Blue Marble Space Institute of Science, Seattle, WA, USA; University of Hawai`i at Mānoa, Mānoa, HI, USA; U.S. Geological Survey, Flagstaff, AZ, USA; University of Winnipeg, Winnipeg, Canada; University of the Basque Country UPV/EHU, Leioa, Bilbao, Spain; Institut de Planétologie et Astrophysique de Grenoble, CNRS, Université Grenoble Alpes, Grenoble, France; Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA; Centre Lasers Intenses et Applications, CNRS, CEA, Université de Bordeaux, Bordeaux, France; Plancius Research, Severna Park, MD, USA; Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France; Laboratoire d'Astrophysique de Bordeaux, CNRS, Université de Bordeaux, Bordeaux, France; Centre National d'Études Spatiales, Toulouse, France; Université de Lyon, UCBL, ENSL, UJM, CNRS, LGL-TPE, Villeurbanne, France; Groupe d'Instrumentation Scientifique, Observatoire Midi-Pyrénées, Toulouse, France; GeoRessources, CNRS, Université de Lorraine, Nancy, France; California Institute of Technology, Pasadena, CA, USA; University of Copenhagen, Copenhagen, Denmark; McGill University, Montreal, Canada; University of Valladolid, Valladolid, Spain; Agencia Estatal Consejo Superior de Investigaciones Científicas, Madrid, Spain; Space Exploration Sector, Johns Hopkins Applied Physics Laboratory, Laurel, MD, USA; Department of Geological Sciences, University of Colorado Boulder, Boulder, CO, USA; University of Maryland, College Park, MD, USA; State University of New York, Stony Brook, NY, USA; Department of Physics and Applied Physics, Kennedy College of Sciences, University of Massachusetts Lowell, Lowell, MA, USA; Institut d'Astrophysique Spatiale, CNRS, Université Paris-Saclay, Orsay, France; Institut Universitaire de France, Paris, France; University of Nevada, Las Vegas, Las Vegas, NV, USA; Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN, USA; Institut de Mécanique des Fluides, Université de Toulouse 3 Paul Sabatier, INP, CNRS, Toulouse, France; Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris, CNRS, Sorbonne Université, Université Paris Diderot, Meudon, France; Laboratoire Atmosphères, Milieux, Observations Spatiales, CNRS, Université Saint-Quentin-en-Yvelines, Sorbonne Université, Guyancourt, France; Universidad de Málaga, Málaga, Spain), ES(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France; Department of Chemistry and Biochemistry, University of South Carolina, Columbia, SC, USA; Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA; Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, CNRS, Sorbonne Université, MNHN, Paris, France; Heliospace Corporation, Berkeley, CA, USA; Haystack Observatory, Massachusetts Institute of Technology, Westford, MA, USA; Department of Aeronautics and Astronautics, Massachusetts Institute of Technology, Cambridge, MA, USA; Laboratoire de Planétologie et Géosciences, CNRS, Nantes Université, Université Angers, Nantes, France; Escuela de Ingeniería de Bilbao, Universidad del País Vasco UPV/EHU, Bilbao, Spain; Aeolis Corporation, Sierra Madre, CA, USA; Centro de Astrobiología (INTA-CSIC), Madrid, Spain; Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA; Deutsches Zentrum für Luft- und Raumfahrt (DLR), Institute of Optical Sensor Systems, Berlin, Germany; Blue Marble Space Institute of Science, Seattle, WA, USA; University of Hawai`i at Mānoa, Mānoa, HI, USA; U.S. Geological Survey, Flagstaff, AZ, USA; University of Winnipeg, Winnipeg, Canada; University of the Basque Country UPV/EHU, Leioa, Bilbao, Spain; Institut de Planétologie et Astrophysique de Grenoble, CNRS, Université Grenoble Alpes, Grenoble, France; Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA; Centre Lasers Intenses et Applications, CNRS, CEA, Université de Bordeaux, Bordeaux, France; Plancius Research, Severna Park, MD, USA; Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France; Laboratoire d'Astrophysique de Bordeaux, CNRS, Université de Bordeaux, Bordeaux, France; Centre National d'Études Spatiales, Toulouse, France; Université de Lyon, UCBL, ENSL, UJM, CNRS, LGL-TPE, Villeurbanne, France; Groupe d'Instrumentation Scientifique, Observatoire Midi-Pyrénées, Toulouse, France; GeoRessources, CNRS, Université de Lorraine, Nancy, France; California Institute of Technology, Pasadena, CA, USA; University of Copenhagen, Copenhagen, Denmark; McGill University, Montreal, Canada; University of Valladolid, Valladolid, Spain; Agencia Estatal Consejo Superior de Investigaciones Científicas, Madrid, Spain; Space Exploration Sector, Johns Hopkins Applied Physics Laboratory, Laurel, MD, USA; Department of Geological Sciences, University of Colorado Boulder, Boulder, CO, USA; University of Maryland, College Park, MD, USA; State University of New York, Stony Brook, NY, USA; Department of Physics and Applied Physics, Kennedy College of Sciences, University of Massachusetts Lowell, Lowell, MA, USA; Institut d'Astrophysique Spatiale, CNRS, Université Paris-Saclay, Orsay, France; Institut Universitaire de France, Paris, France; University of Nevada, Las Vegas, Las Vegas, NV, USA; Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN, USA; Institut de Mécanique des Fluides, Université de Toulouse 3 Paul Sabatier, INP, CNRS, Toulouse, France; Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris, CNRS, Sorbonne Université, Université Paris Diderot, Meudon, France; Laboratoire Atmosphères, Milieux, Observations Spatiales, CNRS, Université Saint-Quentin-en-Yvelines, Sorbonne Université, Guyancourt, France; Universidad de Málaga, Málaga, Spain), ET(Centre National d'Études Spatiales, Toulouse, France), EU(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France; Department of Chemistry and Biochemistry, University of South Carolina, Columbia, SC, USA; Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA; Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, CNRS, Sorbonne Université, MNHN, Paris, France; Heliospace Corporation, Berkeley, CA, USA; Haystack Observatory, Massachusetts Institute of Technology, Westford, MA, USA; Department of Aeronautics and Astronautics, Massachusetts Institute of Technology, Cambridge, MA, USA; Laboratoire de Planétologie et Géosciences, CNRS, Nantes Université, Université Angers, Nantes, France; Escuela de Ingeniería de Bilbao, Universidad del País Vasco UPV/EHU, Bilbao, Spain; Aeolis Corporation, Sierra Madre, CA, USA; Centro de Astrobiología (INTA-CSIC), Madrid, Spain; Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA; Deutsches Zentrum für Luft- und Raumfahrt (DLR), Institute of Optical Sensor Systems, Berlin, Germany; Blue Marble Space Institute of Science, Seattle, WA, USA; University of Hawai`i at Mānoa, Mānoa, HI, USA; U.S. Geological Survey, Flagstaff, AZ, USA; University of Winnipeg, Winnipeg, Canada; University of the Basque Country UPV/EHU, Leioa, Bilbao, Spain; Institut de Planétologie et Astrophysique de Grenoble, CNRS, Université Grenoble Alpes, Grenoble, France; Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA; Centre Lasers Intenses et Applications, CNRS, CEA, Université de Bordeaux, Bordeaux, France; Plancius Research, Severna Park, MD, USA; Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France; Laboratoire d'Astrophysique de Bordeaux, CNRS, Université de Bordeaux, Bordeaux, France; Centre National d'Études Spatiales, Toulouse, France; Université de Lyon, UCBL, ENSL, UJM, CNRS, LGL-TPE, Villeurbanne, France; Groupe d'Instrumentation Scientifique, Observatoire Midi-Pyrénées, Toulouse, France; GeoRessources, CNRS, Université de Lorraine, Nancy, France; California Institute of Technology, Pasadena, CA, USA; University of Copenhagen, Copenhagen, Denmark; McGill University, Montreal, Canada; University of Valladolid, Valladolid, Spain; Agencia Estatal Consejo Superior de Investigaciones Científicas, Madrid, Spain; Space Exploration Sector, Johns Hopkins Applied Physics Laboratory, Laurel, MD, USA; Department of Geological Sciences, University of Colorado Boulder, Boulder, CO, USA; University of Maryland, College Park, MD, USA; State University of New York, Stony Brook, NY, USA; Department of Physics and Applied Physics, Kennedy College of Sciences, University of Massachusetts Lowell, Lowell, MA, USA; Institut d'Astrophysique Spatiale, CNRS, Université Paris-Saclay, Orsay, France; Institut Universitaire de France, Paris, France; University of Nevada, Las Vegas, Las Vegas, NV, USA; Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN, USA; Institut de Mécanique des Fluides, Université de Toulouse 3 Paul Sabatier, INP, CNRS, Toulouse, France; Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris, CNRS, Sorbonne Université, Université Paris Diderot, Meudon, France; Laboratoire Atmosphères, Milieux, Observations Spatiales, CNRS, Université Saint-Quentin-en-Yvelines, Sorbonne Université, Guyancourt, France; Universidad de Málaga, Málaga, Spain), EV(Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA), EW(Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA), EX(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France; Department of Chemistry and Biochemistry, University of South Carolina, Columbia, SC, USA; Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA; Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, CNRS, Sorbonne Université, MNHN, Paris, France; Heliospace Corporation, Berkeley, CA, USA; Haystack Observatory, Massachusetts Institute of Technology, Westford, MA, USA; Department of Aeronautics and Astronautics, Massachusetts Institute of Technology, Cambridge, MA, USA; Laboratoire de Planétologie et Géosciences, CNRS, Nantes Université, Université Angers, Nantes, France; Escuela de Ingeniería de Bilbao, Universidad del País Vasco UPV/EHU, Bilbao, Spain; Aeolis Corporation, Sierra Madre, CA, USA; Centro de Astrobiología (INTA-CSIC), Madrid, Spain; Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA; Deutsches Zentrum für Luft- und Raumfahrt (DLR), Institute of Optical Sensor Systems, Berlin, Germany; Blue Marble Space Institute of Science, Seattle, WA, USA; University of Hawai`i at Mānoa, Mānoa, HI, USA; U.S. Geological Survey, Flagstaff, AZ, USA; University of Winnipeg, Winnipeg, Canada; University of the Basque Country UPV/EHU, Leioa, Bilbao, Spain; Institut de Planétologie et Astrophysique de Grenoble, CNRS, Université Grenoble Alpes, Grenoble, France; Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA; Centre Lasers Intenses et Applications, CNRS, CEA, Université de Bordeaux, Bordeaux, France; Plancius Research, Severna Park, MD, USA; Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France; Laboratoire d'Astrophysique de Bordeaux, CNRS, Université de Bordeaux, Bordeaux, France; Centre National d'Études Spatiales, Toulouse, France; Université de Lyon, UCBL, ENSL, UJM, CNRS, LGL-TPE, Villeurbanne, France; Groupe d'Instrumentation Scientifique, Observatoire Midi-Pyrénées, Toulouse, France; GeoRessources, CNRS, Université de Lorraine, Nancy, France; California Institute of Technology, Pasadena, CA, USA; University of Copenhagen, Copenhagen, Denmark; McGill University, Montreal, Canada; University of Valladolid, Valladolid, Spain; Agencia Estatal Consejo Superior de Investigaciones Científicas, Madrid, Spain; Space Exploration Sector, Johns Hopkins Applied Physics Laboratory, Laurel, MD, USA; Department of Geological Sciences, University of Colorado Boulder, Boulder, CO, USA; University of Maryland, College Park, MD, USA; State University of New York, Stony Brook, NY, USA; Department of Physics and Applied Physics, Kennedy College of Sciences, University of Massachusetts Lowell, Lowell, MA, USA; Institut d'Astrophysique Spatiale, CNRS, Université Paris-Saclay, Orsay, France; Institut Universitaire de France, Paris, France; University of Nevada, Las Vegas, Las Vegas, NV, USA; Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN, USA; Institut de Mécanique des Fluides, Université de Toulouse 3 Paul Sabatier, INP, CNRS, Toulouse, France; Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris, CNRS, Sorbonne Université, Université Paris Diderot, Meudon, France; Laboratoire Atmosphères, Milieux, Observations Spatiales, CNRS, Université Saint-Quentin-en-Yvelines, Sorbonne Université, Guyancourt, France; Universidad de Málaga, Málaga, Spain), EY(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France), EZ(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France; Department of Chemistry and Biochemistry, University of South Carolina, Columbia, SC, USA; Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA; Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, CNRS, Sorbonne Université, MNHN, Paris, France; Heliospace Corporation, Berkeley, CA, USA; Haystack Observatory, Massachusetts Institute of Technology, Westford, MA, USA; Department of Aeronautics and Astronautics, Massachusetts Institute of Technology, Cambridge, MA, USA; Laboratoire de Planétologie et Géosciences, CNRS, Nantes Université, Université Angers, Nantes, France; Escuela de Ingeniería de Bilbao, Universidad del País Vasco UPV/EHU, Bilbao, Spain; Aeolis Corporation, Sierra Madre, CA, USA; Centro de Astrobiología (INTA-CSIC), Madrid, Spain; Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA; Deutsches Zentrum für Luft- und Raumfahrt (DLR), Institute of Optical Sensor Systems, Berlin, Germany; Blue Marble Space Institute of Science, Seattle, WA, USA; University of Hawai`i at Mānoa, Mānoa, HI, USA; U.S. Geological Survey, Flagstaff, AZ, USA; University of Winnipeg, Winnipeg, Canada; University of the Basque Country UPV/EHU, Leioa, Bilbao, Spain; Institut de Planétologie et Astrophysique de Grenoble, CNRS, Université Grenoble Alpes, Grenoble, France; Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA; Centre Lasers Intenses et Applications, CNRS, CEA, Université de Bordeaux, Bordeaux, France; Plancius Research, Severna Park, MD, USA; Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France; Laboratoire d'Astrophysique de Bordeaux, CNRS, Université de Bordeaux, Bordeaux, France; Centre National d'Études Spatiales, Toulouse, France; Université de Lyon, UCBL, ENSL, UJM, CNRS, LGL-TPE, Villeurbanne, France; Groupe d'Instrumentation Scientifique, Observatoire Midi-Pyrénées, Toulouse, France; GeoRessources, CNRS, Université de Lorraine, Nancy, France; California Institute of Technology, Pasadena, CA, USA; University of Copenhagen, Copenhagen, Denmark; McGill University, Montreal, Canada; University of Valladolid, Valladolid, Spain; Agencia Estatal Consejo Superior de Investigaciones Científicas, Madrid, Spain; Space Exploration Sector, Johns Hopkins Applied Physics Laboratory, Laurel, MD, USA; Department of Geological Sciences, University of Colorado Boulder, Boulder, CO, USA; University of Maryland, College Park, MD, USA; State University of New York, Stony Brook, NY, USA; Department of Physics and Applied Physics, Kennedy College of Sciences, University of Massachusetts Lowell, Lowell, MA, USA; Institut d'Astrophysique Spatiale, CNRS, Université Paris-Saclay, Orsay, France; Institut Universitaire de France, Paris, France; University of Nevada, Las Vegas, Las Vegas, NV, USA; Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN, USA; Institut de Mécanique des Fluides, Université de Toulouse 3 Paul Sabatier, INP, CNRS, Toulouse, France; Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris, CNRS, Sorbonne Université, Université Paris Diderot, Meudon, France; Laboratoire Atmosphères, Milieux, Observations Spatiales, CNRS, Université Saint-Quentin-en-Yvelines, Sorbonne Université, Guyancourt, France; Universidad de Málaga, Málaga, Spain), FA(Institut d'Astrophysique Spatiale, CNRS, Université Paris-Saclay, Orsay, France; Institut Universitaire de France, Paris, France), FB(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France), FC(Centre National d'Études Spatiales, Toulouse, France), FD(Institut d'Astrophysique Spatiale, CNRS, Université Paris-Saclay, Orsay, France), FE(Université de Lyon, UCBL, ENSL, UJM, CNRS, LGL-TPE, Villeurbanne, France), FF(Laboratoire d'Astrophysique de Bordeaux, CNRS, Université de Bordeaux, Bordeaux, France), FG(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France), FH(Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA), FI(Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA), FJ(Centre National d'Études Spatiales, Toulouse, France), FK(Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris, CNRS, Sorbonne Université, Université Paris Diderot, Meudon, France), FL(University of Valladolid, Valladolid, Spain), FM(Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, CNRS, Sorbonne Université, MNHN, Paris, France), FN(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France; Department of Chemistry and Biochemistry, University of South Carolina, Columbia, SC, USA; Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA; Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, CNRS, Sorbonne Université, MNHN, Paris, France; Heliospace Corporation, Berkeley, CA, USA; Haystack Observatory, Massachusetts Institute of Technology, Westford, MA, USA; Department of Aeronautics and Astronautics, Massachusetts Institute of Technology, Cambridge, MA, USA; Laboratoire de Planétologie et Géosciences, CNRS, Nantes Université, Université Angers, Nantes, France; Escuela de Ingeniería de Bilbao, Universidad del País Vasco UPV/EHU, Bilbao, Spain; Aeolis Corporation, Sierra Madre, CA, USA; Centro de Astrobiología (INTA-CSIC), Madrid, Spain; Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA; Deutsches Zentrum für Luft- und Raumfahrt (DLR), Institute of Optical Sensor Systems, Berlin, Germany; Blue Marble Space Institute of Science, Seattle, WA, USA; University of Hawai`i at Mānoa, Mānoa, HI, USA; U.S. Geological Survey, Flagstaff, AZ, USA; University of Winnipeg, Winnipeg, Canada; University of the Basque Country UPV/EHU, Leioa, Bilbao, Spain; Institut de Planétologie et Astrophysique de Grenoble, CNRS, Université Grenoble Alpes, Grenoble, France; Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA; Centre Lasers Intenses et Applications, CNRS, CEA, Université de Bordeaux, Bordeaux, France; Plancius Research, Severna Park, MD, USA; Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France; Laboratoire d'Astrophysique de Bordeaux, CNRS, Université de Bordeaux, Bordeaux, France; Centre National d'Études Spatiales, Toulouse, France; Université de Lyon, UCBL, ENSL, UJM, CNRS, LGL-TPE, Villeurbanne, France; Groupe d'Instrumentation Scientifique, Observatoire Midi-Pyrénées, Toulouse, France; GeoRessources, CNRS, Université de Lorraine, Nancy, France; California Institute of Technology, Pasadena, CA, USA; University of Copenhagen, Copenhagen, Denmark; McGill University, Montreal, Canada; University of Valladolid, Valladolid, Spain; Agencia Estatal Consejo Superior de Investigaciones Científicas, Madrid, Spain; Space Exploration Sector, Johns Hopkins Applied Physics Laboratory, Laurel, MD, USA; Department of Geological Sciences, University of Colorado Boulder, Boulder, CO, USA; University of Maryland, College Park, MD, USA; State University of New York, Stony Brook, NY, USA; Department of Physics and Applied Physics, Kennedy College of Sciences, University of Massachusetts Lowell, Lowell, MA, USA; Institut d'Astrophysique Spatiale, CNRS, Université Paris-Saclay, Orsay, France; Institut Universitaire de France, Paris, France; University of Nevada, Las Vegas, Las Vegas, NV, USA; Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN, USA; Institut de Mécanique des Fluides, Université de Toulouse 3 Paul Sabatier, INP, CNRS, Toulouse, France; Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris, CNRS, Sorbonne Université, Université Paris Diderot, Meudon, France; Laboratoire Atmosphères, Milieux, Observations Spatiales, CNRS, Université Saint-Quentin-en-Yvelines, Sorbonne Université, Guyancourt, France; Universidad de Málaga, Málaga, Spain), FO(University of Hawai`i at Mānoa, Mānoa, HI, USA), FP(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA), FQ(Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France), FR(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France; Department of Chemistry and Biochemistry, University of South Carolina, Columbia, SC, USA; Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA; Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, CNRS, Sorbonne Université, MNHN, Paris, France; Heliospace Corporation, Berkeley, CA, USA; Haystack Observatory, Massachusetts Institute of Technology, Westford, MA, USA; Department of Aeronautics and Astronautics, Massachusetts Institute of Technology, Cambridge, MA, USA; Laboratoire de Planétologie et Géosciences, CNRS, Nantes Université, Université Angers, Nantes, France; Escuela de Ingeniería de Bilbao, Universidad del País Vasco UPV/EHU, Bilbao, Spain; Aeolis Corporation, Sierra Madre, CA, USA; Centro de Astrobiología (INTA-CSIC), Madrid, Spain; Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA; Deutsches Zentrum für Luft- und Raumfahrt (DLR), Institute of Optical Sensor Systems, Berlin, Germany; Blue Marble Space Institute of Science, Seattle, WA, USA; University of Hawai`i at Mānoa, Mānoa, HI, USA; U.S. Geological Survey, Flagstaff, AZ, USA; University of Winnipeg, Winnipeg, Canada; University of the Basque Country UPV/EHU, Leioa, Bilbao, Spain; Institut de Planétologie et Astrophysique de Grenoble, CNRS, Université Grenoble Alpes, Grenoble, France; Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA; Centre Lasers Intenses et Applications, CNRS, CEA, Université de Bordeaux, Bordeaux, France; Plancius Research, Severna Park, MD, USA; Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France; Laboratoire d'Astrophysique de Bordeaux, CNRS, Université de Bordeaux, Bordeaux, France; Centre National d'Études Spatiales, Toulouse, France; Université de Lyon, UCBL, ENSL, UJM, CNRS, LGL-TPE, Villeurbanne, France; Groupe d'Instrumentation Scientifique, Observatoire Midi-Pyrénées, Toulouse, France; GeoRessources, CNRS, Université de Lorraine, Nancy, France; California Institute of Technology, Pasadena, CA, USA; University of Copenhagen, Copenhagen, Denmark; McGill University, Montreal, Canada; University of Valladolid, Valladolid, Spain; Agencia Estatal Consejo Superior de Investigaciones Científicas, Madrid, Spain; Space Exploration Sector, Johns Hopkins Applied Physics Laboratory, Laurel, MD, USA; Department of Geological Sciences, University of Colorado Boulder, Boulder, CO, USA; University of Maryland, College Park, MD, USA; State University of New York, Stony Brook, NY, USA; Department of Physics and Applied Physics, Kennedy College of Sciences, University of Massachusetts Lowell, Lowell, MA, USA; Institut d'Astrophysique Spatiale, CNRS, Université Paris-Saclay, Orsay, France; Institut Universitaire de France, Paris, France; University of Nevada, Las Vegas, Las Vegas, NV, USA; Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN, USA; Institut de Mécanique des Fluides, Université de Toulouse 3 Paul Sabatier, INP, CNRS, Toulouse, France; Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris, CNRS, Sorbonne Université, Université Paris Diderot, Meudon, France; Laboratoire Atmosphères, Milieux, Observations Spatiales, CNRS, Université Saint-Quentin-en-Yvelines, Sorbonne Université, Guyancourt, France; Universidad de Málaga, Málaga, Spain), FS(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France), FT(University of the Basque Country UPV/EHU, Leioa, Bilbao, Spain), FU(University of Winnipeg, Winnipeg, Canada), FV(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France; Department of Chemistry and Biochemistry, University of South Carolina, Columbia, SC, USA; Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA; Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, CNRS, Sorbonne Université, MNHN, Paris, France; Heliospace Corporation, Berkeley, CA, USA; Haystack Observatory, Massachusetts Institute of Technology, Westford, MA, USA; Department of Aeronautics and Astronautics, Massachusetts Institute of Technology, Cambridge, MA, USA; Laboratoire de Planétologie et Géosciences, CNRS, Nantes Université, Université Angers, Nantes, France; Escuela de Ingeniería de Bilbao, Universidad del País Vasco UPV/EHU, Bilbao, Spain; Aeolis Corporation, Sierra Madre, CA, USA; Centro de Astrobiología (INTA-CSIC), Madrid, Spain; Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA; Deutsches Zentrum für Luft- und Raumfahrt (DLR), Institute of Optical Sensor Systems, Berlin, Germany; Blue Marble Space Institute of Science, Seattle, WA, USA; University of Hawai`i at Mānoa, Mānoa, HI, USA; U.S. Geological Survey, Flagstaff, AZ, USA; University of Winnipeg, Winnipeg, Canada; University of the Basque Country UPV/EHU, Leioa, Bilbao, Spain; Institut de Planétologie et Astrophysique de Grenoble, CNRS, Université Grenoble Alpes, Grenoble, France; Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA; Centre Lasers Intenses et Applications, CNRS, CEA, Université de Bordeaux, Bordeaux, France; Plancius Research, Severna Park, MD, USA; Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France; Laboratoire d'Astrophysique de Bordeaux, CNRS, Université de Bordeaux, Bordeaux, France; Centre National d'Études Spatiales, Toulouse, France; Université de Lyon, UCBL, ENSL, UJM, CNRS, LGL-TPE, Villeurbanne, France; Groupe d'Instrumentation Scientifique, Observatoire Midi-Pyrénées, Toulouse, France; GeoRessources, CNRS, Université de Lorraine, Nancy, France; California Institute of Technology, Pasadena, CA, USA; University of Copenhagen, Copenhagen, Denmark; McGill University, Montreal, Canada; University of Valladolid, Valladolid, Spain; Agencia Estatal Consejo Superior de Investigaciones Científicas, Madrid, Spain; Space Exploration Sector, Johns Hopkins Applied Physics Laboratory, Laurel, MD, USA; Department of Geological Sciences, University of Colorado Boulder, Boulder, CO, USA; University of Maryland, College Park, MD, USA; State University of New York, Stony Brook, NY, USA; Department of Physics and Applied Physics, Kennedy College of Sciences, University of Massachusetts Lowell, Lowell, MA, USA; Institut d'Astrophysique Spatiale, CNRS, Université Paris-Saclay, Orsay, France; Institut Universitaire de France, Paris, France; University of Nevada, Las Vegas, Las Vegas, NV, USA; Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN, USA; Institut de Mécanique des Fluides, Université de Toulouse 3 Paul Sabatier, INP, CNRS, Toulouse, France; Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris, CNRS, Sorbonne Université, Université Paris Diderot, Meudon, France; Laboratoire Atmosphères, Milieux, Observations Spatiales, CNRS, Université Saint-Quentin-en-Yvelines, Sorbonne Université, Guyancourt, France; Universidad de Málaga, Málaga, Spain), FW(University of Nevada, Las Vegas, Las Vegas, NV, USA), FX(University of Valladolid, Valladolid, Spain), FY(Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA), FZ(Deutsches Zentrum für Luft- und Raumfahrt (DLR), Institute of Optical Sensor Systems, Berlin, Germany)
Journal:	Nature, Volume 605, Issue 7911, p.653-658.
Publication Date:	Apr 2022
Origin:	Springer Science and Business Media LLC
DOI:	https://doi.org/10.1038/s41586-022-04679-0
Bibliographic Code:	2022Natur.605..653M
Abstract:	Before the Perseverance rover landing, the acoustic environment of Mars was unknown. Models predicted that: (1) atmospheric turbulence changes at centimetre scales or smaller at the point where molecular viscosity converts kinetic energy into heat<SUP>1</SUP>, (2) the speed of sound varies at the surface with frequency<SUP>2,3</SUP> and (3) high-frequency waves are strongly attenuated with distance in CO<SUB>2</SUB> (refs. <SUP>2-4</SUP>). However, theoretical models were uncertain because of a lack of experimental data at low pressure and the difficulty to characterize turbulence or attenuation in a closed environment. Here, using Perseverance microphone recordings, we present the first characterization of the acoustic environment on Mars and pressure fluctuations in the audible range and beyond, from 20 Hz to 50 kHz. We find that atmospheric sounds extend measurements of pressure variations down to 1,000 times smaller scales than ever observed before, showing a dissipative regime extending over five orders of magnitude in energy. Using point sources of sound (Ingenuity rotorcraft, laser-induced sparks), we highlight two distinct values for the speed of sound that are about 10 m s<SUP>‒1</SUP> apart below and above 240 Hz, a unique characteristic of low-pressure CO<SUB>2</SUB>-dominated atmosphere. We also provide the acoustic attenuation with distance above 2 kHz, allowing us to explain the large contribution of the CO<SUB>2</SUB> vibrational relaxation in the audible range. These results establish a ground truth for the modelling of acoustic processes, which is critical for studies in atmospheres such as those of Mars and Venus.

Title:	Characteristics of convective vortices and dust devils at gale crater on Mars during MY33
Authors:	Uttam, Shefali; Sheel, Varun; Singh, D.; Newman, C. E.; Lemmon, M. T.
Affiliation:	AA(Physical Research Laboratory, Navarangpura, Ahmedabad, 380009, India), AB(Physical Research Laboratory, Navarangpura, Ahmedabad, 380009, India), AC(Physical Research Laboratory, Navarangpura, Ahmedabad, 380009, India), AD(Aeolis Research, Pasadena, CA, USA), AE(Space Science Institute, Boulder, USA)
Journal:	Planetary and Space Science, Volume 213, article id. 105430.
Publication Date:	Apr 2022
Origin:	Elsevier BV
Keywords:	Martian atmosphere, Convective vortex, Dust devils
Abstract Copyright:	(c) 2022 Elsevier Ltd
DOI:	https://doi.org/10.1016/j.pss.2022.105430
Bibliographic Code:	2022P&SS..21305430U
Abstract:	Convective vortices that are dust laden (dust devils), are believed to be an efficient mechanism for particle entrainment in the Martian atmosphere. Such vortices can be identified in-situ by landers or rovers by the reduced surface pressure when they pass by the instrument. We analyse data from the Rover Environmental Monitoring Station (REMS) on-board the Mars Science Laboratory (MSL) rover Curiosity during mission sols 1019 to 1686 (corresponding to Martian Year (MY) 33). We identified 611 short pressure drops that likely indicate the passage of convective vortices in vicinity of the rover. The cumulative power-law analysis of the detected pressure drops suggests a low abundance of stronger pressure drop events at the MSL site as compared to the Pathfinder and Phoenix sites. The reason for this can be attributed to the smaller boundary layer height at Gale crater. The power-law slope is smaller for MY 33 as compared to previous years, suggesting that the dust devil activity also increased inside the Gale crater with the progressing year. Among all vortices detected, 63 vortices (∼10%) also show a simultaneous drop in ultraviolet intensity, which signifies obscuration of sunlight by the dust-laden vortices. A seasonal study for dust devils occurrences based on UV flux data shows an increase in their frequency during the local southern summer season. A majority of our estimated tangential wind velocities are well below the Martian dust lifting threshold. This indicates that either the vortices passed far from the measuring instrument or that the threshold being used is higher than the actual threshold on Mars.

Title:	Winter Weakening of Titan's Stratospheric Polar Vortices
Authors:	Shultis, J.; Waugh, D. W.; Toigo, A. D.; Newman, C. E.; Teanby, N. A.; Sharkey, J.
Affiliation:	AA(Department of Earth and Planetary Sciences, Johns Hopkins University, Baltimore, MD 21210, USA), AB(Department of Earth and Planetary Sciences, Johns Hopkins University, Baltimore, MD 21210, USA), AC(Johns Hopkins Applied Physics Laboratory, MD, USA), AD(Aeolis Research, USA), AE(School of Earth Sciences, University of Bristol, Bristol, UK), AF(School of Earth Sciences, University of Bristol, Bristol, UK)
Journal:	The Planetary Science Journal, Volume 3, Issue 4, id.73, <NUMPAGES>11</NUMPAGES> pp.
Publication Date:	Apr 2022
Origin:	American Astronomical Society
Keywords:	Atmospheric science, Planetary atmospheres, Atmospheric circulation, Titan, Saturnian satellites, Stratosphere, 116, 1244, 112, 2186, 1427, 1640
DOI:	https://doi.org/10.3847/PSJ/ac5ea1
Bibliographic Code:	2022PSJ.....3...73S
Abstract:	Polar vortices are a prominent feature in Titan's stratosphere. The Cassini mission has provided a detailed view of the breakdown of the northern polar vortex and formation of the southern vortex, but the mission did not observe the full annual cycle of the evolution of the vortices. Here we use a TitanWRF general circulation model simulation of an entire Titan year to examine the full annual cycle of the polar vortices. The simulation reveals a winter weakening of the vortices, with a clear minimum in polar potential vorticity and midlatitude zonal winds between winter solstice and spring equinox. The simulation also produces the observed postfall equinox cooling followed by rapid warming in the upper stratosphere. This warming is due to strong descent and adiabatic heating, which also leads to the formation of an annular potential vorticity structure. The seasonal evolution of the polar vortices is very similar in the two hemispheres, with only small quantitative differences that are much smaller than the seasonal variations, which can be related to Titan's orbital eccentricity. This suggests that any differences between observations of the northern hemisphere vortex in late northern winter and the southern hemisphere vortex in early winter are likely due to the different observation times with respect to solstice, rather than fundamental differences in the polar vortices.

Title:	Diurnal Variability in Aeolian Sediment Transport at Gale Crater, Mars
Authors:	Baker, Mariah M.; Newman, Claire E.; Sullivan, Robert; Minitti, Michelle E.; Edgett, Kenneth S.; Fey, Deirdra; Ellison, Doug; Lewis, Kevin W.
Affiliation:	AA(Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, Washington, DC USA; Morton K. Blaustein Department of Earth and Planetary Sciences, The Johns Hopkins University, Baltimore, MD USA), AB(Aeolis Research, Pasadena, CA USA), AC(Department of Astronomy, Cornell University, Ithaca, NY USA), AD(Framework, Silver Spring, MD USA), AE(Malin Space Science Systems, San Diego, CA USA), AF(Malin Space Science Systems, San Diego, CA USA), AG(NASA's Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA), AH(Morton K. Blaustein Department of Earth and Planetary Sciences, The Johns Hopkins University, Baltimore, MD USA)
Journal:	Journal of Geophysical Research: Planets, Volume 127, Issue 2, article id. e06734.
Publication Date:	Feb 2022
Origin:	American Geophysical Union (AGU)
Keywords:	aeolian activity, saltation dynamics, Martian circulation patterns, Gale crater, Mars, curiosity rover
Abstract Copyright:	2022. American Geophysical Union. All Rights Reserved.
DOI:	https://doi.org/10.1029/2020JE006734
Bibliographic Code:	2022JGRE..12706734B
Abstract:	A suite of high resolution cameras onboard the Mars Science Laboratory (MSL) Curiosity rover have provided an unparalleled look at active aeolian processes on Mars, including within the first active dune field explored on another planet, the Bagnold Dunes. Here we present results from a subset of MSL's repeat imaging ("change detection") experiments with temporal resolutions sufficient to probe the diurnal variability in winds within Gale crater. Images reveal that saltation is a near-daily phenomenon during southern summer, with repeatable diurnal circulation patterns producing steady impact ripple migration toward the west/southwest. Nighttime fluxes are inferred to be ∼four times larger than daytime fluxes, consistent with predictions from the MarsWRF model of multiple periods of enhanced wind between sunset and sunrise. Multiple factors are likely facilitating saltation at this time: (a) time-averaged nighttime winds have a higher degree of variance (i.e., higher peak friction speeds) than daytime winds, (b) interactions between regional Hadley flows and local, thermally driven slope winds cause increased turbulence at night, and (c) relatively higher atmospheric density produces correspondingly higher shear stresses and decreases critical thresholds. Observations of sand transport at a range of spatiotemporal scales (down to scale of individual particles moving on the timescale of seconds) support the idea that bedform migration is driven by intermittent, low-flux saltation events when winds fluctuate between canonical impact and fluid thresholds. Yet, whereas gustiness may play a role in initiating transport, saltation is found to be highly predictable on diurnal timescales and is only stochastic on the shortest timescales characteristic of turbulent fluctuations in wind.