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2025

Title: Rapid Decay of Martian Global Dust Storms Driven by Small-Scale Deposition Processes in the Lower Planetary Boundary Layer
Authors: Li, Lulu; Sun, Cong; Newman, Claire E.; Fan, Siteng; Zhao, Yongxuan; Li, Tao; Zhao, Chun
Affiliation: AA(National Key Laboratory of Deep Space Exploration/School of Earth and Space Sciences/Institute of Advanced Interdisciplinary Research on High‐Performance Computing Systems and Software, University of Science and Technology of China, Hefei, China; Department of Earth and Space Sciences, Southern University of Science and Technology, Shenzhen, China;), AB(Department of Earth and Space Sciences, Southern University of Science and Technology, Shenzhen, China), AC(Aeolis Research, Chandler, AZ, USA;), AD(Department of Earth and Space Sciences, Southern University of Science and Technology, Shenzhen, China;), AE(National Key Laboratory of Deep Space Exploration/School of Earth and Space Sciences/Institute of Advanced Interdisciplinary Research on High‐Performance Computing Systems and Software, University of Science and Technology of China, Hefei, China), AF(National Key Laboratory of Deep Space Exploration/School of Earth and Space Sciences/Institute of Advanced Interdisciplinary Research on High‐Performance Computing Systems and Software, University of Science and Technology of China, Hefei, China;), AG(National Key Laboratory of Deep Space Exploration/School of Earth and Space Sciences/Institute of Advanced Interdisciplinary Research on High‐Performance Computing Systems and Software, University of Science and Technology of China, Hefei, China; Laoshan Laboratory, Qingdao, China; CAS Center for Excellence in Comparative Planetology, University of Science and Technology of China, Hefei, China;)
Journal: Geophysical Research Letters, Volume 52, Issue 22, id.e2025GL118229, 10 pp.
Publication Date: Nov 2025
Origin: American Geophysical Union (AGU)
Keywords: MarsWRF, global dust storm, dry deposition, radiative-dynamic feedback
Abstract Copyright: © 2025. The Author(s).
DOI: https://doi.org/10.1029/2025GL118229
Bibliographic Code: 2025GeoRL..5218229L
Abstract: As one of the iconic features on Mars, global dust storms (GDSs) often decay rapidly. However, general circulation models (GCMs) typically underestimate their decay rates, which is one of the major challenges in simulating the Martian atmosphere. Here, we evaluate the role of a recently implemented size-resolved microphysical deposition scheme of dust particles in the MarsWRF model on GDS evolution. This scheme includes a series of microphysical processes, in addition to gravitational sedimentation, which facilitates the efficient removal of small dust particles. The model successfully reproduces the observed increase in effective particle radius during dust storms, along with their rapid decay. A radiative-dynamic positive feedback loop is seen among solar insolation, atmospheric stability, dust lifting and dissipation, and atmospheric dynamics. These results highlight the role of microphysics in the development of planetary-scale events on Mars, and underscore the need to include small-scale processes in Mars GCMs.
Title: Detection of triboelectric discharges during dust events on Mars
Authors: Chide, Baptiste; Lorenz, Ralph D.; Montmessin, Franck; Maurice, Sylvestre; Parot, Yann; Hueso, Ricardo; Martinez, German; Vicente-Retortillo, Alvaro; Jacob, Xavier; Lemmon, Mark; Dubois, Bruno; Meslin, Pierre-Yves; Newman, Claire; Bertrand, Tanguy; Deprez, Grégoire; Toledo, Daniel; Sánchez-Lavega, Agustin; Cousin, Agnès; Wiens, Roger C.
Affiliation: AA(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse, CNRS, CNES, Toulouse, France ;), AB(Space Exploration Sector, Johns Hopkins Applied Physics Laboratory, Laurel, MD, USA ;), AC(Laboratoire Atmosphères, Milieux, Observations Spatiale, CNRS, Université Saint-Quentin-en-Yvelines, Sorbonne Université, Guyancourt, France ;), AD(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse, CNRS, CNES, Toulouse, France), AE(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse, CNRS, CNES, Toulouse, France), AF(Física Aplicada, Escuela de Ingeniería de Bilbao, University of the Basque Country (UPV/EHU), Bilbao, Spain ;), AG(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AH(Centro de Astrobiología (INTA-CSIC), Madrid, Spain ;), AI(Institut de Mécanique des Fluides, Université de Toulouse, INP, CNRS, Toulouse, France), AJ(Space Science Institute, Boulder, CO, USA), AK(Observatoire Midi-Pyrénées, Université de Toulouse, Toulouse, France), AL(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse, CNRS, CNES, Toulouse, France), AM(Aeolis Research, Chandler, AZ, USA ; Ulster University, Coleraine, UK ;), AN(LIRA, Observatoire de Paris, Université PSL, Sorbonne Université, Université Paris Cité, CY Cergy Paris Université, CNRS, Meudon, France ;), AO(European Space Research and Technology Centre (ESTEC), European Space Agency, Noordwijk, The Netherlands), AP(Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain ;), AQ(Física Aplicada, Escuela de Ingeniería de Bilbao, University of the Basque Country (UPV/EHU), Bilbao, Spain ;), AR(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse, CNRS, CNES, Toulouse, France ;), AS(Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN, USA ;)
Journal: Nature, Volume 647, Issue 8091, pp. 865-869.
Publication Date: Nov 2025
Origin: Springer Science and Business Media LLC
Abstract Copyright: © The Author(s), under exclusive licence to Springer Nature Limited 2025
DOI: https://doi.org/10.1038/s41586-025-09736-y
Bibliographic Code: 2025Natur.647..865C
Abstract: Lightning is among the most energetic manifestation of electrical activity in planetary atmospheres, with documented observations not only on Earth but also on Saturn and Jupiter<SUP>1</SUP>. On Mars, the existence of electrical activity has long been suspected<SUP>2,3</SUP> but never directly demonstrated. The dusty atmosphere of Mars undergoes aeolian processes, ranging from wind-blown dust and sand, metre-to-hundred-metre-sized dust devils to thousand-kilometre-scale dust storms<SUP>4</SUP>, which, in Earth's deserts, can become electrified through triboelectric charging<SUP>5, 6─7</SUP>. For this reason, electric fields have been predicted to build up on Mars<SUP>8, 9─10</SUP>, but with no measurement of Martian atmospheric electrical activity so far. Here we report in situ detections of triboelectric discharges, identified by their electrical and acoustic signatures captured by the SuperCam microphone aboard the Perseverance rover<SUP>11,12</SUP>. Fifty-five events have been detected over two Martian years, usually associated with dust devils and dust storm convective fronts. These serendipitous observations demonstrate that Martian electric fields can reach the breakdown threshold of the near-surface atmosphere of Mars, predicted to be on the order of several tens of kV m<SUP>−1</SUP>. Such electrical activity could affect dust dynamics<SUP>13,14</SUP> and potentially fuel a reactive electrochemical environment enhancing the oxidizing capacity of the atmosphere, with consequences for the preservation of organic molecules<SUP>15,16</SUP>. This in situ evidence may have implications for surface chemistry, habitability and human exploration.
Title: The Feedback of Atmospheric Dust Tides on Migrating Thermal Tides During Martian Major Dust Storms: A Model Study Based on MarsWRF
Authors: Cheng, Yueming; Wu, Zhaopeng; Lian, Yuan; Cui, Jun; Wei, Yong
Affiliation: AA(Planetary Environmental and Astrobiological Research Laboratory (PEARL), School of Atmospheric Sciences, Sun Yat‐Sen University, Zhuhai, China;), AB(Key Laboratory of Planetary Science and Frontier Technology, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing, China;), AC(Aeolis Research, Chandler, AZ, USA), AD(Planetary Environmental and Astrobiological Research Laboratory (PEARL), School of Atmospheric Sciences, Sun Yat‐Sen University, Zhuhai, China;), AE(Key Laboratory of Planetary Science and Frontier Technology, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing, China; College of Earth and Planetary Sciences, University of Chinese Academy of Sciences, Beijing, China;)
Journal: Journal of Geophysical Research: Planets, Volume 130, Issue 11, id.e2024JE008914, 24 pp.
Publication Date: Nov 2025
Origin: American Geophysical Union (AGU)
Keywords: Martian atmosphere, GCM simulation, dust storm, tides
Abstract Copyright: © 2025. American Geophysical Union. All Rights Reserved.
DOI: https://doi.org/10.1029/2024JE008914
Bibliographic Code: 2025JGRE..13008914C
Abstract: Previous studies revealed intense diurnal variations in dust opacity in the southern hemisphere during major dust storms on Mars. This short-term dust variation is also referred to as 'dust tides' due to its violent north-south diurnal motion, which is driven by strong meridional tidal winds. Given the pivotal role of airborne dust in Martian climate, it is imperative to assess the dynamical impact of dust tides. This study focuses on the feedback between dust tides and atmospheric thermal tides on Mars during major dust storms, employing the MarsWRF General Circulation Model. In order to evaluate the impact of dust tides on atmospheric thermal tides, we compare two scenarios: "dust tide" and "no dust tide." The former accounts for diurnal dust variations, whereas the latter utilizes daily-averaged dust distributions. The results of our simulations indicate that the inclusion of diurnal dust variations leads to a notable increase in the amplitude of Martian atmospheric migrating diurnal and semidiurnal tides. The enhanced atmospheric diurnal tides can reinforce the diurnal dust variations through the increased meridional wind, thereby establishing a positive feedback mechanism. Sensitivity experiments, including both latitudinal amplitude variations and phase-shifted scenarios, demonstrate that Martian atmospheric diurnal tides respond linearly to the latitudinal extent of dust tides. Moreover, the feedback efficiency is strongly modulated by the local time of dust enhancement, with phase alignment between dust-induced heating and tidal oscillations being critical for effective amplification. These results imply that even modest latitudinal variations in dust opacity, if aligned with tidal oscillations, can be further amplified during major dust storms. These findings highlight the necessity of incorporating short-term dust variations in climate models to accurately predict Martian atmospheric behaviors during dust storms.
Title: How does topography affect wind abrasion on Mars? Recently observed shifts in ventifact orientation at Gale crater
Authors: Zhou, Daniel Y.; Turner, Madison L.; Rapin, William; Schieber, Juergen; Roberts, Amelie L.; Cowart, Aster C.; Hoffman, Megan E.; Hallet, Bernard; Banham, Steve G.; Fey, Deirdra; Lewis, Kevin W.; Gupta, Sanjeev; Newman, Claire E.; Vasavada, Ashwin R.; Weitz, Cathy M.; Dietrich, William E.; Grant, John A.; Viúdez-Moreiras, Daniel; Kite, Edwin S.
Affiliation: AA(Department of the Geophysical Sciences, University of Chicago, Chicago, IL 60637, USA), AB(Department of the Geophysical Sciences, University of Chicago, Chicago, IL 60637, USA), AC(Institut de Recherche en Astrophysique et Planétologie, BP 44346 31028, Toulouse Cedex 4, France), AD(Department of Geological Sciences, Indiana University, Bloomington, IN 47408, USA), AE(Department of Earth Science &amp; Engineering, Imperial College London, London SW7 2BP, UK), AF(Planetary Science Institute, Tucson, AZ 85719, USA), AG(Department of Geology, University of New Mexico, Albuquerque, NM 87131, USA), AH(Department of Earth and Space Sciences, University of Washington, Seattle, WA 98195, USA), AI(Department of Earth Science &amp; Engineering, Imperial College London, London SW7 2BP, UK), AJ(Malin Space Science Systems, San Diego, CA 92191, USA), AK(Department of Earth and Planetary Science, Johns Hopkins University, Baltimore, MD 21218, USA), AL(Department of Earth Science &amp; Engineering, Imperial College London, London SW7 2BP, UK), AM(Aeolis Research, Chandler, AZ 85224, USA), AN(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91011, USA), AO(Planetary Science Institute, Tucson, AZ 85719, USA), AP(Department of Earth &amp; Planetary Science, University of California, Berkeley, CA 94720, USA), AQ(Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, Washington, DC 20560, USA), AR(Centro de Astrobiología, National Institute for Aerospace Technology, 28850 Torrejón de Ardoz, Madrid, Spain), AS(Department of the Geophysical Sciences, University of Chicago, Chicago, IL 60637, USA)
Journal: Icarus, Volume 437, id.116605.
Publication Date: Sep 2025
Origin: Elsevier BV
Keywords: Mars, Planetary geology, Geological processes
Abstract Copyright: © 2025 Elsevier Inc. All rights are reserved, including those for text and data mining, AI training, and similar technologies.
DOI: https://doi.org/10.1016/j.icarus.2025.116605
Bibliographic Code: 2025Icar..43716605Z
Abstract: Wind abrasion is the dominant erosive process inferred from observations by Curiosity during its traverse in Gale crater, but how and how fast wind scours Mount Sharp is unclear. Here, we infer formative wind direction from ventifacts (wind-eroded rock fragments) measured from Curiosity's recent traverse. We compare these measurements to previous ones and to wind model predictions, and attempt to estimate the current rate of wind erosion near Curiosity's location on Mount Sharp. Ventifacts in this study indicate winds blowing south-southeast, agreeing with previous studies on the floor of Gale crater, but differing from studies at the base of the mountain slope. Upslope abrasive wind flows predominate, consistent with idealized models. At some sites, ventifacts are oriented both upslope and downslope on Mount Sharp, suggesting bimodal wind direction at the mountain, agreeing with circulation models that predict diurnal reversals. Using crater-retention age statistics at one site, we estimate a ∼ 3.5 ± 0.8 μm/Earth year (yr) upslope horizontal erosion rate at Mount Sharp. We suggest the observed ventifacts formed when Mars' obliquity and climate regime were similar to those in the present day.
Title: The role of planetary-scale waves on the stratospheric superrotation in Titan's atmosphere
Authors: Lian, Yuan; Leung, Cecilia; Newman, Claire; Tamppari, Leslie
Affiliation: AA(Aeolis Research, Chandler, AZ, United States of America), AB(NASA JPL, Pasadena, CA, United States of America), AC(Aeolis Research, Chandler, AZ, United States of America), AD(NASA JPL, Pasadena, CA, United States of America)
Journal: Icarus, Volume 435, id.116561.
Publication Date: Jul 2025
Origin: Elsevier BV
Keywords: Titan atmosphere, Planetary waves, Superrotation, Atmospheric instabilities, Wave analysis, Earth and Planetary Astrophysics, Atmospheric and Oceanic Physics
Abstract Copyright: © 2025 Elsevier Inc. All rights are reserved, including those for text and data mining, AI training, and similar technologies.
DOI: https://doi.org/10.1016/j.icarus.2025.116561
Bibliographic Code: 2025Icar..43516561L
Abstract: We analyze simulation results from the TitanWRF global circulation model to understand the mechanisms that maintain the equatorial superrotation in Titan's stratosphere. We find that the eddies associated with wave activities can transport angular momentum upgradient to zonal flow, leading to acceleration of the equatorial superrotation. The dominant wave modes identified in this study are consistent with previous studies, with zonal wavenumber 1 being the major contributor to the prograde acceleration. Despite the same conclusion of maintenance of equatorial superrotation via wave-mean interactions, we find that the way waves interact with the zonal flow in TitanWRF is slightly different from some other studies. We confirm our previous findings that in TitanWRF this occurs primarily during a dozen or so annual, short-duration (a few Titan sols) angular momentum "transfer events," which have a repeatable seasonal pattern but differ slightly in timing and magnitude between years. This is not the case in the Titan Atmosphere Model (TAM), which found milder angular momentum transfers that produced the strongest acceleration of superrotation around solstice in the upper stratosphere and more continuous year-around acceleration in the lower stratosphere. Despite differences in angular momentum transfer across models, we further find that, similar to the TAM wave analysis results, eddies generated by Rossby-Kelvin instabilities may be the major source of prograde angular momentum for the equatorial superrotation, although TitanWRF may also include contributions from the absorption of vertically propagating equatorial Kelvin waves. This differs from our previous work, which suggested barotropic waves were responsible for TitanWRF's solsticial transfer event.
Title: Surface Dust Coverages on Rock Targets in Gale Crater: Influence of Elevation, Proximity to Aeolian Sand Fields and Seasonality
Authors: Henley, T. L. J.; Schmidt, M. E.; Lewis, K. W.; Moores, J. E.; Hayes, C.; Bray, S. L.; Bradley, N. J.; Lee, R. E.; Marincic, I. K.; Turner, K. W.; Guzewich, S. D.; Newman, C. E.; Bischof, G.; Viúdez-Moreiras, D.
Affiliation: AA(Earth Science Department, Brock University, St. Catharines, ON, Canada;), AB(Earth Science Department, Brock University, St. Catharines, ON, Canada;), AC(Department of Earth &amp; Planetary Sciences, Johns Hopkins University, Baltimore, MD, USA;), AD(Centre for Research in Earth and Space Science, York University, Toronto, ON, Canada;), AE(Centre for Research in Earth and Space Science, York University, Toronto, ON, Canada;), AF(Earth Science Department, Brock University, St. Catharines, ON, Canada), AG(Earth Science Department, Brock University, St. Catharines, ON, Canada), AH(Earth Science Department, Brock University, St. Catharines, ON, Canada), AI(Earth Science Department, Brock University, St. Catharines, ON, Canada), AJ(Earth Science Department, Brock University, St. Catharines, ON, Canada), AK(NASA Goddard Space Flight Center, Greenbelt, MD, USA;), AL(C.E. ─ Aeolis Research, Tuscon, AZ, USA;), AM(Centre for Research in Earth and Space Science, York University, Toronto, ON, Canada;), AN(Centro de Astrobiología (CSIC-INTA) and National Institute for Aerospace Technology (INTA), Madrid, Spain;)
Journal: Journal of Geophysical Research: Planets, Volume 130, Issue 7, id.e2023JE008184, 19 pp.
Publication Date: Jul 2025
Origin: American Geophysical Union (AGU)
Keywords: Mars, dust, seasons, surface processes, particle mobility
Abstract Copyright: © 2025. The Author(s).
DOI: https://doi.org/10.1029/2023JE008184
Bibliographic Code: 2025JGRE..13008184H
Abstract: Martian dust is mobilized throughout the year by local, regional, and global dust storms, influencing atmospheric opacity and inhibiting observations of the surface. Using Mars Hand Lens Imager (MAHLI) images and methods of Schmidt et al. (2018), https://doi.org/10.1029/2018je005553, areal dust coverages on 368 near-horizontal, undisturbed rock surfaces were estimated along six Mars Years of the Mars Science Laboratory (MSL) Curiosity rover's geologic traverse from mission sols 46─3,409, corresponding to Mars Year 31 (MY#; Clancy et al., 2000, https://doi.org/10.1029/1999JE001089), areocentric solar longitude (Ls) 175.9° through MY36, Ls 177.6°. Targets were evaluated for potential geospatial and seasonal (Ls) correlations. Dust coverages increased at each spring equinox (Ls = 0°) with the highest coverage (76.6%) recorded at the top of Vera Rubin Ridge (VRR) prior to the Mars Year 34 (MY34) global dust storm. Dust coverages annually decreased as prevailing wind strengths in the Gale crater increased during southern summer. Following the ascent of VRR, New Year maximums have decreased by approximately 15% annually (MY35 60.7%, and MY36 52.8%), suggesting that dust is less abundant at higher elevations on Mount Sharp, and/or that dust suspension or removal is enhanced at higher elevations by stronger winds at higher elevations. Two regions with relatively low dust coverages (&lt;20%) were found in proximity to active aeolian sand dunes and are interpreted to result from saltating sand particles striking and lofting dust particles. This research represents the single longest recording of surface dust deposits to date for landed missions.
Title: Dust Lifting and Deposition Over Six Mars Years at Gale Crater, Mars, From REMS Observations and Mesoscale Simulations
Authors: Vicente-Retortillo, A.; Martinez, G. M.; Newman, C. E.; Lemmon, M. T.; Johnson, J. R.; Mason, E. L.; Renno, N. O.; Rodriguez-Manfredi, J. A.
Affiliation: AA(Centro de Astrobiologia (INTA-CSIC), Madrid, Spain;), AB(Centro de Astrobiologia (INTA-CSIC), Madrid, Spain;), AC(Aeolis Research, Chandler, AZ, USA;), AD(Space Science Institute, Boulder, CO, USA;), AE(Johns Hopkins University Applied Physics Laboratory, Laurel, MD, USA;), AF(Northern Arizona University, Flagstaff, AZ, USA), AG(University of Michigan, Ann Arbor, MI, USA), AH(Centro de Astrobiologia (INTA-CSIC), Madrid, Spain)
Journal: Journal of Geophysical Research: Planets, Volume 130, Issue 6, id.e2024JE008888, 18 pp.
Publication Date: Jun 2025
Origin: American Geophysical Union (AGU)
Keywords: Mars, dust lifting, dust accumulation, Mars science laboratory, REMS, MarsWRF
Abstract Copyright: © 2025. The Author(s).
DOI: https://doi.org/10.1029/2024JE008888
Bibliographic Code: 2025JGRE..13008888V
Abstract: We present the temporal evolution of the effect of dust accumulation on two surfaces of the Curiosity rover at Gale crater during almost 4,000 sols using Rover Environmental Monitoring Station (REMS), Chemcam and Mastcam observations, and compare it with simulations of the Mars Weather Research and Forecasting Model (MarsWRF) atmospheric numerical model and environmental observations to improve our understanding of dust lifting on Mars. After almost six full Mars Years (MY), dust accumulated on the REMS UV sensor (UVS) attenuates an average of 45% of the incoming radiation. Dust accumulation on the UVS follows a seasonal cycle with gradual dust accumulation during the aphelion season followed by dust removal until L<SUB>s</SUB> ∼ 300°. However, there is a strong interannual variability during the dusty season. MarsWRF simulations show that wind stress has a strong diurnal, seasonal and interannual variability; simulations of dust devil activity show a seasonal pattern that aligns with pressure drop observations, peaking also at L<SUB>s</SUB> ∼ 300°. Dust lifting mechanisms are variable, with a larger relative importance of wind stress in MY 31 and 32, and of dust devils in MY 34 to 36. Dust accumulation on the Chemcam calibration target follows a very similar temporal evolution, but with a marked offset since the 2018 Global Dust Storm, suggesting that surface tilt is particularly important around intense dust storms. We characterize dust lifting mechanisms at Gale crater and quantify the effect of dust accumulation during an extraordinary dust storm on different surfaces; the observed net removal periods validate MarsWRF simulations and suggest the suitability of Gale Crater for long-term solar-powered missions.
Title: Impacts of Dry Deposition Processes With Resolved Dust Particle Sizes on Simulating the Martian Dust
Authors: Li, Lulu; Zhao, Chun; Newman, Claire E.; Zhao, Yongxuan; Feng, Jiawang; Li, Tao; Yang, Chengyun; Yue, Yingxi
Affiliation: AA(Deep Space Exploration Laboratory/School of Earth and Space Sciences, CMA-USTC Laboratory of Fengyun Remote Sensing, State Key Laboratory of Fire Science, Institute of Advanced Interdisciplinary Research on High-Performance Computing Systems and Software, University of Science and Technology of China, Hefei, China;), AB(Deep Space Exploration Laboratory/School of Earth and Space Sciences, CMA-USTC Laboratory of Fengyun Remote Sensing, State Key Laboratory of Fire Science, Institute of Advanced Interdisciplinary Research on High-Performance Computing Systems and Software, University of Science and Technology of China, Hefei, China; Laoshan Laboratory, Qingdao, China; CAS Center for Excellence in Comparative Planetology, University of Science and Technology of China, Hefei, China;), AC(Aeolis Research, Chandler, AZ, USA;), AD(Deep Space Exploration Laboratory/School of Earth and Space Sciences, CMA-USTC Laboratory of Fengyun Remote Sensing, State Key Laboratory of Fire Science, Institute of Advanced Interdisciplinary Research on High-Performance Computing Systems and Software, University of Science and Technology of China, Hefei, China), AE(Deep Space Exploration Laboratory/School of Earth and Space Sciences, CMA-USTC Laboratory of Fengyun Remote Sensing, State Key Laboratory of Fire Science, Institute of Advanced Interdisciplinary Research on High-Performance Computing Systems and Software, University of Science and Technology of China, Hefei, China;), AF(Deep Space Exploration Laboratory/School of Earth and Space Sciences, CMA-USTC Laboratory of Fengyun Remote Sensing, State Key Laboratory of Fire Science, Institute of Advanced Interdisciplinary Research on High-Performance Computing Systems and Software, University of Science and Technology of China, Hefei, China;), AG(Deep Space Exploration Laboratory/School of Earth and Space Sciences, CMA-USTC Laboratory of Fengyun Remote Sensing, State Key Laboratory of Fire Science, Institute of Advanced Interdisciplinary Research on High-Performance Computing Systems and Software, University of Science and Technology of China, Hefei, China;), AH(Deep Space Exploration Laboratory/School of Earth and Space Sciences, CMA-USTC Laboratory of Fengyun Remote Sensing, State Key Laboratory of Fire Science, Institute of Advanced Interdisciplinary Research on High-Performance Computing Systems and Software, University of Science and Technology of China, Hefei, China)
Journal: Journal of Geophysical Research: Planets, Volume 130, Issue 5, id.e2024JE008616, 31 pp.
Publication Date: May 2025
Origin: American Geophysical Union (AGU)
Keywords: dry deposition, Martian dust, resolved particle sizes, MarsWRF
Abstract Copyright: © 2025. American Geophysical Union. All Rights Reserved.
DOI: https://doi.org/10.1029/2024JE008616
Bibliographic Code: 2025JGRE..13008616L
Abstract: Mars, characterized as a "desert" planet with little water vapor, primarily relies on dry deposition for dust removal. Although these processes include gravitational sedimentation, turbulent transfer, Brownian diffusion, impaction, interception, and rebound, most current models consider only gravitational sedimentation. To have a more comprehensive understanding of the effects of Martian dust removal processes, a physics-based scheme of dry deposition processes with resolved dust particle sizes is implemented in the Mars Weather Research and Forecasting (MarsWRF) model. Results show that the size-resolved dry deposition scheme significantly increases the dry deposition velocity, with the maximum difference (over 0.024 m/s) occurring at 0.884 μm size bin. This enhanced removal efficiency leads to an increase of 0.4 μm in the effective radius of airborne dust throughout the year and a reduction of approximately 0.09 in dust opacity, particularly in the northern high latitudes during autumn and winter, compared to the simulation that only considers a size-resolved gravitational sedimentation scheme. The overestimation of low-level atmospheric temperature in the mid-to-low latitudes, excluding near-surface regions between $20\mathit{{}^{\circ}}$ and $60\mathit{{}^{\circ}}$N, during ${L}_{s}=230-250\mathit{{}^{\circ}}$ (considered as peak-dust phase) is partially corrected, with a correction of up to 1 K compared to the single-particle size simulation and up to 5 K compared to the size-resolved sedimentation-only simulation, bringing it closer to MCS observations. Additionally, the size-resolved dry deposition simulation reduces the condensation rate of atmospheric CO<SUB>2</SUB> and the thickness of the northern CO<SUB>2</SUB> ice cap, aligning better with Viking Lander observations during northern winter and spring than the size-resolved sedimentation-only simulation.
Title: WindSightNet: The Inter-Annual Variability of Martian Winds Retrieved From InSight's Seismic Data With Machine Learning
Authors: Stott, Alexander E.; Garcia, Raphael F.; Murdoch, Naomi; Mimoun, David; Drilleau, Mélanie; Newman, Claire; Spiga, Aymeric; Banfield, Don; Lemmon, Mark; Navarro, Sara; Mora-Sotomayor, Luis; Charalambous, Constantinos; Pike, William T.; Lognonné, Philippe; Banerdt, William B.
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(Institut Supérieur de l'Aéronautique et de l'Espace (ISAE‐SUPAERO), Université de Toulouse, Toulouse, France;), AF(Aeolis Research, Chandler, AZ, USA;), AG(Laboratoire de Météorologie Dynamique/IPSL, Sorbonne Université, CNRS, Ecole Normale Supérieure, PSL Research University, Ecole Polytechnique, Paris, France;), AH(NASA Ames, Mountain View, CA, USA), AI(Space Science Institute, Boulder, CO, USA;), AJ(Centro de Astrobiologia (CAB), CSIC‐INTA, Madrid, Spain), AK(Centro de Astrobiologia (CAB), CSIC‐INTA, Madrid, Spain;), AL(Department of Electrical and Electronic Engineering, Imperial College London, London, UK;), AM(Department of Electrical and Electronic Engineering, Imperial College London, London, UK), AN(Université de Paris, Institut de physique du globe de Paris, CNRS, Paris, France;), AO(Jet Propulsion Laboratory ─ California Institute of Technology, Pasadena, CA, USA;)
Journal: Journal of Geophysical Research: Planets, Volume 130, Issue 2, page 2024JE008695, 24 pp.
Publication Date: Feb 2025
Origin: American Geophysical Union (AGU)
Keywords: mars, winds, machine learning, atmospheric dynamics
Abstract Copyright: © 2025. The Author(s).
DOI: https://doi.org/10.1029/2024JE008695
Bibliographic Code: 2025JGRE..13008695S
Abstract: Wind measurements from landed missions on Mars are vital to characterize the near surface atmospheric behavior on Mars and improve atmospheric models. These winds are responsible for aeolian change and the mixing of dust in and out of the atmosphere, which has a significant effect on global circulation. The NASA InSight mission recorded wind data for around 750 sols. The seismometer, however, recorded data for around 1400 sols. The dominant source of energy in the seismic data is in fact due to winds. To this end, we propose a machine learning model, dubbed WindSightNet, to map the seismic data to wind speed and direction. The trained network achieves wind speed and direction measurements with errors of 0.932 m/s and 32.6°. We use WindSightNet to retrieve winds from the entire time the seismometer was recording to compare year-to-year wind variations at InSight. The continuous nature of the data set enables the extraction of periodic behavior. We observe a pattern of waves due to baroclinic activity with periods of ${\sim} $2─3, ${\sim} $4, ${\sim} $5─7 and ${\sim} $9─20 sols occurring ${L}_{s}=$180─360°. We also observe periodicity during the day due to convective cells. This is used to estimate the boundary layer height, yielding values between 2.3 and 7.7 km. A data-science based metric is proposed to provide a quantification of the year-to-year differences in the wind speeds. This highlights variations linked to dust activity as well as other transient differences. On the whole, the seismic-derived winds confirm the dominance of the global circulation leading to repeatable weather patterns.
Title: Collection and In Situ Analyses of Regolith Samples by the Mars 2020 Rover: Implications for Their Formation and Alteration History
Authors: Hausrath, E. M.; Sullivan, R.; Goreva, Y.; Zorzano, M. P.; Vaughan, A.; Cousin, A.; Siljeström, S.; Sharma, S.; Shumway, A. O.; Kizovski, T.; VanBommel, S. J.; Tice, M.; Knight, A.; Martinez, G.; Vicente-Retortillo, A.; Mandon, L.; Adcock, C. T.; Madariaga, J. M.; Población, I.; Johnson, J. R.; Lasue, J.; Gasnault, O.; Randazzo, N.; Cardarelli, E. L.; Kronyak, R.; Bechtold, A.; Paar, G.; Udry, A.; Forni, O.; Bedford, C. C.; Carman, N. A.; Bell, J. F.; Benison, K.; Bosak, T.; Brown, A.; Broz, A.; Calef, F.; Clark, B. C.; Cloutis, E.; Czaja, A. D.; Fornaro, T.; Fouchet, T.; Golombek, M.; Gómez, F.; Herd, C. D. K.; Herkenhoff, K.; Jakubek, R. S.; Jandura, L.; Martinez-Frias, J.; Mayhew, L. E.; Meslin, P.-Y.; Newman, C. E.; Núñez, J. I.; Poulet, F.; Royer, C.; Russell, P.; Sephton, M. A.; Sharma, S. K.; Shuster, D.; Simon, J. I.; Tirona, I.; Wiens, R. C.; Weiss, B. P.; Williams, A. J.; Williford, K.; Wolf, Z. U.
Affiliation: AA(Department of Geoscience, University of Nevada, Las Vegas, NV, USA;), AB(CCAPS, Cornell University, Ithaca, NY, USA;), AC(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA;), AD(Centro de Astrobiologia (CAB), CSIC‐INTA, Torrejón de Ardoz, Spain;), AE(Apogee Engineering, LLC, Flagstaff, AZ, USA;), AF(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France;), AG(RISE Research Institutes of Sweden, Stockholm, Sweden), AH(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA), AI(Department of Earth and Space Sciences, University of Washington, Seattle, WA, USA;), AJ(Department of Earth Science, Brock University, St. Catharines, ON, Canada), AK(Department of Earth and Planetary Sciences, Washington University in St. Louis, St. Louis, MO, USA), AL(Texas A&M University, College Station, TX, USA), AM(Department of Earth and Planetary Sciences, Washington University in St. Louis, St. Louis, MO, USA;), AN(Centro de Astrobiologia (CAB), CSIC‐INTA, Torrejón de Ardoz, Spain; Lunar and Planetary Institute, Houston, TX, USA;), AO(Centro de Astrobiologia (CAB), CSIC‐INTA, Torrejón de Ardoz, Spain;), AP(Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA, USA), AQ(Department of Geoscience, University of Nevada, Las Vegas, NV, USA;), AR(Department of Analytical Chemistry, University of the Basque Country UPV/EHU, Leioa, Spain;), AS(Department of Analytical Chemistry, University of the Basque Country UPV/EHU, Leioa, Spain), AT(Johns Hopkins University Applied Physics Laboratory, Laurel, MD, USA;), AU(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France;), AV(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France;), AW(Department of Earth and Atmospheric Sciences, University of Alberta, Edmonton, AB, Canada), AX(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA; University of California, Los Angeles, Los Angeles, CA, USA;), AY(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA), AZ(Department of Lithospheric Research, University of Vienna, Wien, Austria;), BA(Joanneum Research, Graz, Austria;), BB(Department of Geoscience, University of Nevada, Las Vegas, NV, USA;), BC(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France), BD(Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN, USA;), BE(Department of Geoscience, University of Nevada, Las Vegas, NV, USA;), BF(Arizona State University, Tempe, AZ, USA), BG(Department of Geology and Geography, West Virginia University, Morgantown, WV, USA;), BH(Department of Earth, Atmospheric, and Planetary Science, Massachusetts Institute of Technology, Cambridge, MA, USA;), BI(Plancius Research, Severna Park, MD, USA;), BJ(Joanneum Research, Graz, Austria;), BK(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA;), BL(Space Science Institute, Boulder, CO, USA;), BM(University of Winnipeg, Winnipeg, MB, Canada;), BN(Department of Geosciences, University of Cincinnati, Cincinnati, OH, USA;), BO(INAF—Astrophysical Observatory of Arcetri, Firenze, Italy;), BP(LESIA, Observatoire de Paris, Université PSL, Sorbonne Université, Université Paris Cité, CNRS, Meudon, France;), BQ(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA), BR(Centro de Astrobiologia (CAB), CSIC‐INTA, Torrejón de Ardoz, Spain;), BS(Department of Earth and Atmospheric Sciences, University of Alberta, Edmonton, AB, Canada;), BT(US Geological Survey Astrogeology Science Center, Flagstaff, AZ, USA;), BU(Jacobs, NASA Johnson Space Center, Houston, TX, USA), BV(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA), BW(Institute of Geosciences, IGEO (CSIC‐UCM), Madrid, Spain;), BX(Department of Geological Sciences, University of Colorado Boulder, Boulder, CO, USA;), BY(Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France), BZ(Aeolis Research, Chandler, AZ, USA;), CA(Johns Hopkins University Applied Physics Laboratory, Laurel, MD, USA;), CB(IAS, CNRS/Unversité Paris Saclay, Orsay Cedex, France), CC(Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN, USA), CD(University of California, Los Angeles, Los Angeles, CA, USA;), CE(Department of Earth Science &amp; Engineering, Imperial College, London, UK;), CF(University of Hawaii, Honolulu, HI, USA;), CG(University of California, Berkeley, Berkeley, CA, USA), CH(NASA Johnson Space Center, Houston, TX, USA;), CI(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA;), CJ(Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN, USA;), CK(Department of Earth, Atmospheric, and Planetary Science, Massachusetts Institute of Technology, Cambridge, MA, USA;), CL(Department of Geological Sciences, University of Florida, Gainesville, FL, USA;), CM(Blue Marble Space Institute of Science, Seattle, WA, USA), CN(Los Alamos National Laboratory, Los Alamos, NM, USA; For Members See Appendix A)
Journal: Journal of Geophysical Research: Planets, Volume 130, Issue 2, page 2023JE008046, 51 pp.
Publication Date: Feb 2025
Origin: American Geophysical Union (AGU)
Keywords: Mars regolith samples, dust, soil crust, fluorescence emitters, astrobiology, human exploration
Abstract Copyright: © 2025 The Author(s). 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/10.1029/2023JE008046
Bibliographic Code: 2025JGRE..13008046H
Abstract: The Perseverance rover has sampled mm-size lithic fragments containing olivine likely from at least two source regions from the surface of an inactive megaripple surface, and fine-grained material from the surface and to a depth of ∼4─6 cm. Some of the mm-size grains lack a coherent diffraction pattern measured by PIXL, consistent with the presence of poorly ordered secondary phases that have been altered. Analysis of these materials on Earth will allow examination of materials that have experienced aqueous, potentially habitable environments that could contain biosignatures. Fluorescence of three different patterns was detected, consistent with inorganic emissions from silica defects or rare earth elements in certain mineral phases, although organic origin cannot be excluded. Analysis of Autofocus Context Imager and Wide Angle Topographic Sensor for Operations and eNgineering images of the subsurface material and MEDA thermal inertia measurements indicate average grain sizes of ∼125 and ∼150 μm, respectively, for the bulk material within the megaripple. The fine-grained material in the sampling location indicates chemical compositions similar to previously proposed global components as well as airfall dust. In situ and associated atmospheric measurements provide evidence of recent processes likely including water vapor in soil crust formation. The sampled material will therefore help elucidate the formation of Martian soils; current surface-atmosphere interactions; the composition, shape, and size distribution of dust grains valuable for studies of past and present Martian climate and for assessing potential health and other risks to human missions; and ancient, aqueously altered environments that could have been habitable, and, if Mars contained life, possibly contain biosignatures.
Title: Martian Atmospheric Disturbances From Orbital Images and Surface Pressure at Jezero Crater, Mars, During Martian Year 36
Authors: Sánchez-Lavega, A.; Larsen, E.; del Rio-Gaztelurrrutia, T.; Hernández-Bernal, J.; Ordóñez-Etxebarría, I.; Hueso, R.; Tanguy, B.; Lemmon, M.; Juarez, M. de la Torre; Martínez, G. M.; Munguira, A.; Rodríguez-Manfredi, J. A.; Harri, A.-M.; Pla-García, J.; Toledo, D.; Newman, C.
Affiliation: AA(Escuela de Ingeniería de Bilbao, Universidad País Vasco, UPV/EHU, Bilbao, Spain;), AB(Escuela de Ingeniería de Bilbao, Universidad País Vasco, UPV/EHU, Bilbao, Spain;), AC(Escuela de Ingeniería de Bilbao, Universidad País Vasco, UPV/EHU, Bilbao, Spain;), AD(Laboratoire de Méteorologie Dynamique, Sorbonne Université, Paris, France;), AE(Planetario de Pamplona, Pamplona, Spain), AF(Escuela de Ingeniería de Bilbao, Universidad País Vasco, UPV/EHU, Bilbao, Spain;), AG(LESIA, Observatoire de Paris, Meudon, France), AH(Space Science Institute, College Station, TX, USA;), AI(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA;), AJ(Lunar and Planetary Institute, Houston, TX, USA; Centro de Astrobiología (INTA-CSIC), Madrid, Spain;), AK(Escuela de Ingeniería de Bilbao, Universidad País Vasco, UPV/EHU, Bilbao, Spain;), AL(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AM(Finnish Meteorological Institute, Helsinki, Finland;), AN(Centro de Astrobiología (INTA-CSIC), Madrid, Spain;), AO(Instituto Nacional de Técnica Aeroespacial, INTA, Madrid, Spain;), AP(Aeolis Research, Chandler, AZ, USA;)
Journal: Journal of Geophysical Research: Planets, Volume 130, Issue 1, page 2024JE008565, 26 pp.
Publication Date: Jan 2025
Origin: American Geophysical Union (AGU)
Keywords: planet, mars, atmosphere, dynamics, tides, cyclones, Astrophysics - Earth and Planetary Astrophysics
Abstract Copyright: © 2025 The Author(s).
DOI: https://doi.org/10.1029/2024JE008565
Bibliographic Code: 2025JGRE..13008565S
Abstract: We present a study of atmospheric disturbances at Jezero Crater, Mars, using ground-based measurements of surface pressure by the Perseverance rover in combination with orbital images from the Mars Express and Mars Reconnaissance Orbiter missions. The study starts at L<SUB>s</SUB> ∼ 13.3° in MY36 (6 March 2021) and extends up to L<SUB>s</SUB> ∼ 30.3° in MY37 (28 February 2023). We focus on the characterization of the major atmospheric phenomena at synoptic and planetary-scales. These are the thermal tides (measured up to the sixth component), long-period pressure oscillations (periods &gt;1 sol), the Aphelion Cloud Belt, and the occasional development of regional dust storms over Jezero. We present the seasonal evolution of the amplitudes and phases of the thermal tides and their relation with the atmospheric dust content (optical depth). Three regional dust storms and one polar storm extending over Jezero produced an increase in the diurnal and semidiurnal amplitudes but resulted in inverse responses in their phases. We show that the primary regular wave activity is due to baroclinic disturbances with periods of 2─4 sols and amplitudes ∼ 1─15 Pa increasing with dust content, in good agreement with theoretical predictions by model calculations. The spacecraft images show a number of arc-shaped, spiral and irregular cyclonic vortices, traced by dust and clouds at the edge of the North Polar Cap, that could be behind some of the pressure oscillations measured at Jezero.
Title: Profiling Near-surface Winds on Mars Using Attitude Data from Mars 2020 Ingenuity
Authors: Jackson, Brian; Fenton, Lori; Brown, Travis; Munguira, Asier; Martinez, German; Newman, Claire; Viúdez-Moreiras, Daniel; Golombek, Matthew; Lorenz, Ralph; Paton, Mark D.; Conway, Dylan
Affiliation: AA(Department of Physics, Boise State University, 1910 University Drive, Boise, ID 83725-1570, USA; Carl Sagan Center, SETI Institute, Mountain View, CA, USA), AB(Carl Sagan Center, SETI Institute, Mountain View, CA, USA), AC(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA), AD(Universidad del País Vasco UPV/EHU, Bilbao, Spain), AE(Lunar and Planetary Institute, 3600 Bay Area Boulevard, Office 2029, Houston, TX 77058, USA; Centro de Astrobiologia (CAB, CSIC-INTA) and National Institute for Aerospace Technology (INTA), Madrid, Spain), AF(Aeolis Research, Tucson, AZ, USA), AG(Centro de Astrobiologia (CAB, CSIC-INTA) and National Institute for Aerospace Technology (INTA), Madrid, Spain), AH(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA), AI(Johns Hopkins Applied Physics Laboratory, 1100 Johns Hopkins Road, Laurel, MD, USA), AJ(Finnish Meteorological Institute, PO Box 503, FIN-00101 Helsinki, Finland), AK(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA)
Journal: The Planetary Science Journal, Volume 6, Issue 1, id.21, 20 pp.
Publication Date: Jan 2025
Origin: American Astronomical Society
Keywords: Planetary atmospheres, Mars, 1244, 1007, Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract Copyright: © 2025. The Author(s). Published by the American Astronomical Society.
DOI: https://doi.org/10.3847/PSJ/ad8b41
Bibliographic Code: 2025PSJ.....6...21J
Abstract: We used attitude data from the Mars Ingenuity helicopter with a simple steady-state model to estimate wind speeds and directions at altitudes between 3 and 24 m, the first time winds at such altitudes have been probed on Mars. We compared our estimates to wind data from the meteorology package MEDA on board the Mars 2020 Perseverance rover and to predictions from meteorological models. Wind directions inferred from Ingenuity data agreed with the directions measured by MEDA, when the latter were available, but deviated from model-predicted directions by as much as 180° in some cases. The inferred wind speeds are often much higher than expected. For example, meteorological predictions suggest that Ingenuity should not have seen wind speeds above about 15 m s<SUP>−1</SUP> during its 59th flight, but we inferred speeds reaching nearly 25 m s<SUP>−1</SUP>. For flights during which we have MEDA data to compare to, inferred wind speeds imply friction velocities &gt;1 m s<SUP>−1</SUP> and roughness lengths &gt;10 cm, which seem implausibly large. These results suggest that Ingenuity was probing winds sensitive to aerodynamic conditions hundreds of meters upwind instead of the conditions very near Mars 2020, but they may also reflect a need for updated boundary layer wind models. An improved model for Ingenuity's aerodynamic response that includes the effects of transient winds may also modify our results. In any case, the work here provides a foundation for exploration of planetary boundary layers using drones and suggests important future avenues for research and development.

2024

Title: Evaluation of the InSightSeers and DART Boarders mission observer programmes
Authors: Fernando, Benjamin; Newman, Claire; Daubar, Ingrid J.; Beghein, Caroline; Chabot, Nancy L.; Irving, Jessica C. E.; Johnson, Catherine L.; Panning, Mark P.; Plesa, Ana-Catalina; Rivkin, Andrew S.; Smrekar, Sue; Banerdt, W. Bruce
Affiliation: AA(Department of Earth and Planetary Sciences, Johns Hopkins University, Baltimore, MD, USA), AB(Aeolis Research, Chandler, AZ, USA), AC(Department of Earth, Environmental and Planetary Sciences, Brown University, Providence, RI, USA), AD(Department of Earth, Planetary, and Space Sciences, University of California Los Angeles, Los Angeles, CA, USA), AE(Space Exploration Sector, Johns Hopkins University Applied Physics Laboratory, Laurel, MD, USA), AF(School of Earth Sciences, University of Bristol, Bristol, UK), AG(Department of Earth, Ocean, and Atmospheric Sciences, University of British Columbia, Vancouver, British Columbia, Canada; Planetary Science Institute, Tuscon, AZ, USA), AH(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA), AI(Institute of Planetary Research, German Aerospace Center (DLR), Berlin, Germany), AJ(Space Exploration Sector, Johns Hopkins University Applied Physics Laboratory, Laurel, MD, USA), AK(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA), AL(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA)
Journal: Nature Astronomy, Volume 8, p. 1521-1528.
Publication Date: Dec 2024
Origin: Springer Science and Business Media LLC
Abstract Copyright: 2024: Springer Nature Limited
DOI: https://doi.org/10.1038/s41550-024-02434-1
Bibliographic Code: 2024NatAs...8.1521F
Abstract: Encouraging diversity in planetary science requires making a particular effort to bring a broader range of people onto the mission teams that are the backbone of the field. Observer programmes, which offer early-career researchers the chance to embed within a mission team during a science meeting, are one way of doing this. Here we present a quantitative analysis of the effectiveness of two observer programmes: InSightSeers and DART Boarders, linked respectively to the InSight and the Double Asteroid Redirection Test (DART) missions, using a mixture of one-group pre-test/post-test and one-group post-test only evaluation methods, with a total of 56 participants. We find substantial educational value added to participants from both programmes, with particular strengths being the effectiveness of these programmes at providing an introduction to mission teams and international collaborations. This work demonstrates that mission observer programmes can be an effective way of exposing early-career researchers to planetary science missions.
Title: Distinct Energy Budgets of Mars and Earth
Authors: Guan, Larry; Li, Liming; Creecy, Ellen C.; Jiang, Xun; Wang, Xinyue; Martínez, Germán; Toigo, Anthony D.; Richardson, Mark I.; Sánchez-Lavega, Agustín; Lee, Yeon Joo
Affiliation: AA(Department of Physics, University of Houston, Houston, TX, USA;), AB(Department of Physics, University of Houston, Houston, TX, USA;), AC(Department of Earth and Atmospheric Sciences, University of Houston, Houston, TX, USA), AD(Department of Earth and Atmospheric Sciences, University of Houston, Houston, TX, USA), AE(Department of Earth and Atmospheric Sciences, University of Houston, Houston, TX, USA;), AF(Lunar and Planetary Institute, Houston, TX, USA;), AG(Applied Physics Laboratory, Johns Hopkins University, Laurel, MD, USA), AH(Aeolis Research, Chandler, AZ, USA), AI(Departamento Física Aplicada, Universidad Del País Vasco, Bilbao, Spain;), AJ(PRC for Climate and Earth Science, Institute for Basic Science, Daejeon, South Korea)
Journal: AGU Advances, Volume 5, Issue 6, page 2024AV001389, 14 pp.
Publication Date: Dec 2024
Origin: American Geophysical Union (AGU)
Keywords: energy budget, Mars, Earth, Mars lobal surveyor, thermal emission spectrometer, radiometry
Abstract Copyright: © 2024. The Author(s).
DOI: https://doi.org/10.1029/2024AV001389
Bibliographic Code: 2024AGUA....501389G
Abstract: The radiant energy budget (REB) is a fundamental physical parameter for planetary bodies, though studies constraining the REB for bodies beyond Earth are relatively limited. We generate the first meridional profiles of Mars' REB at seasonal and annual timescales through measurements based on long term multi-instrument observations from spacecraft orbiting Mars. Then, we compare our findings to Earth's REB using contemporary satellite data sets. Each planet exhibits remarkably distinct seasonal REB distributions due to differences in their orbital, atmospheric, and surface properties. Annually, Earth's REB exhibits a tropical energy surplus and a deficit at the poles. In contrast, Mars' annual REB displays an inverted meridional distribution with significant hemispheric asymmetry. Additionally, global dust storms significantly modify the Martian REB. Our observations are employable in future studies to improve models on Mars' general circulation, meteorology, and polar ice cap evolution.
Title: Drying of the Martian mesosphere during aphelion induced by lower temperatures
Authors: Toledo, Daniel; Rannou, Pascal; Apéstigue, Victor; Rodriguez-Veloso, Raul; Arruego, Ignacio; Martínez, German; Tamppari, Leslie; Munguira, Asier; Lorenz, Ralph; Stcherbinine, Aurélien; Montmessin, Franck; Sanchez-Lavega, Agustin; Patel, Priya; Smith, Michael; Lemmon, Mark; Vicente-Retortillo, Alvaro; Newman, Claire; Viudez-Moreiras, Daniel; Hueso, Ricardo; Bertrand, Tanguy; Pla-Garcia, Jorge; Yela, Margarita; de la Torre Juarez, Manuel; Rodriguez-Manfredi, Jose Antonio
Affiliation: AA(Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain ;), AB(GSMA, UMR 7331-GSMA, Universite de Reims Champagne-Ardenne, 51687, Reims, France), AC(Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain), AD(Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain), AE(Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain ;), AF(Lunar and Planetary Institute, Universities Space Research Association, Houston, TX, USA ;), AG(Jet Propulsion Laboratory, CAlifornia Institute of Technology, Pasadena, CA, USA), AH(Universidad del País Vasco UPV/EHU, Bilbao, Spain ;), AI(Johns Hopkins Applied Physics Laboratory, Laurel, MD, USA ;), AJ(IRAP - Institut de Recherche en Astrophysique et Planétologie, Toulouse, France ;), AK(Laboratoire Atmosphàres Milieux Observations Spatiales (LATMOS), Universitá Paris-Saclayz, Sorbonne Universitá, Centre National de la Recherche Scientifique, Guyancourt, France;), AL(Universidad del País Vasco UPV/EHU, Bilbao, Spain ;), AM(Jet Propulsion Laboratory, CAlifornia Institute of Technology, Pasadena, CA, USA), AN(NASA Godard Space Flight Center, Greenbelt, MD, USA), AO(Space Science Institute, Boulder, CO, USA), AP(Centro de Atrobiología (INTA-CSIC), Torrejón de Ardoz, Madrid, Spain), AQ(Aeolis Research, Chandler, AZ, USA ;), AR(Centro de Atrobiología (INTA-CSIC), Torrejón de Ardoz, Madrid, Spain ;), AS(Universidad del País Vasco UPV/EHU, Bilbao, Spain ;), AT(LESIA, Observatoire de Paris, Meudon, France ;), AU(Centro de Atrobiología (INTA-CSIC), Torrejón de Ardoz, Madrid, Spain), AV(Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain), AW(Jet Propulsion Laboratory, CAlifornia Institute of Technology, Pasadena, CA, USA), AX(Centro de Atrobiología (INTA-CSIC), Torrejón de Ardoz, Madrid, Spain ;)
Journal: Communications Earth &amp; Environment, Volume 5, Issue 1, id.717.
Publication Date: Nov 2024
Origin: Springer Science and Business Media LLC
Abstract Copyright: © The Author(s) 2024
DOI: https://doi.org/10.1038/s43247-024-01878-7
Bibliographic Code: 2024ComEE...5..717T
Abstract: The formation of water ice clouds or hazes on Mars imposes substantial limitations on the vertical transport of water into the middle-upper atmosphere, impacting the planet's hydrogen loss. Recent observations made by the Mars Environmental Dynamics Analyzer instrument onboard Mars 2020 Perseverance rover have shown a marked decline in water ice abundance within the mesosphere (above 35-40 km) when Mars is near its aphelion (near the northern summer solstice), notably occurring during solar longitudes (Ls) between Ls 70<SUP>∘</SUP> and 80<SUP>∘</SUP>. Orbital observations around the same latitudes indicate that temperatures between ~ 30-40 km reach a minimum during the same period. Using cloud microphysics simulations, we demonstrate that this decrease in temperature effectively increases the amount of water cold-trapped at those altitudes, confining water ice condensation to lower altitudes. Similarly, the reinforcement of the cold trap induced by the lower temperatures results in significant reductions in the water vapor mixing ratio above 35-40 km, explaining the confinement of water vapor observed around aphelion from orbiters.
Title: Large Scale Oscillations in the Martian Tropical Cloud Belt
Authors: Wang, Huiqun; Richardson, Mark I.; Toigo, Anthony D.; Newman, Claire E.
Affiliation: AA(Center for Astrophysics, Harvard-Smithsonian, Cambridge, MA USA), AB(Aeolis Research, Chandler, AZ USA), AC(John Hopkins University Applied Physics Laboratory, Laurel, MD USA), AD(Aeolis Research, Chandler, AZ USA)
Journal: Journal of Geophysical Research: Planets, Volume 129, Issue 10, article id. e2024JE008479.
Publication Date: Oct 2024
Origin: American Geophysical Union (AGU)
Keywords: Mars, clouds, waves, Mars daily global map, Martian atmosphere, tropical cloud belt
Abstract Copyright: 2024. American Geophysical Union. All Rights Reserved.
DOI: https://doi.org/10.1029/2024JE008479
Bibliographic Code: 2024JGRE..12908479W
Abstract: The Tropical Cloud Oscillation (TCO) in the Martian atmosphere is a shift of clouds in the northern spring and summer tropical cloud belt between the eastern and western hemispheres on an intra-seasonal timescale of about 10-40 sols. The TCO is a significant intraseasonal variation and may strongly affect the Martian general circulation, water cycle, and dust cycle. We examine TCOs using multiple data sets with a focus on the clouds observed in Mars Daily Global Maps during Mars Year (MY) 29-35. One or more TCO cycles are observed in each MY and the phenomenon is most prominent during L<SUB>s</SUB> = 135°-185°. Space-time spectral analysis shows a variety of waves which appear to follow the theoretical dispersion relationships of equatorial waves, such as Kelvin waves, Rossby waves, and Mixed Rossby Gravity waves. The TCO appears to be controlled by zonal wavenumber one traveling waves with Kelvin and Rossby wave characteristics and exhibits a fine-scale latitudinal structure that requires modeling with sufficient resolution. Issues with current data assimilation products for use in studies of Martian equatorial waves due to this fine-scale structure are discussed.
Title: Dust Accumulation and Lifting at the Landing Site of the Mars 2020 Mission, Jezero Crater, as Observed From MEDA
Authors: Vicente-Retortillo, A.; Lemmon, M. T.; Martinez, G. M.; Toledo, D.; Apéstigue, V.; Arruego, I.; Bertrand, T.; Lorenz, R.; Sebastián, E.; Hueso, R.; Newman, C.; Smith, M. D.; Rodriguez-Manfredi, J. A.
Affiliation: AA(Centro de Astrobiología (CAB), CSIC-INTA, Torrejón de Ardoz, Spain), AB(Space Science Institute, Boulder, CO USA), AC(Lunar and Planetary Institute, Universities Space Research Association, Houston, TX USA), AD(Instituto Nacional de Técnica Aeroespacial (INTA), Torrejón de Ardoz, Spain), AE(Instituto Nacional de Técnica Aeroespacial (INTA), Torrejón de Ardoz, Spain), AF(Instituto Nacional de Técnica Aeroespacial (INTA), Torrejón de Ardoz, Spain), AG(LESIA, Paris Observatory, Meudon, France), AH(JHU/APL, Laurel, MD USA), AI(Centro de Astrobiología (CAB), CSIC-INTA, Torrejón de Ardoz, Spain), AJ(Universidad del País Vasco UPV/EHU, Bilbao, Spain), AK(Aeolis Research, Chandler, AZ USA), AL(NASA Goddard Space Flight Center, Greenbelt, MD USA), AM(Centro de Astrobiología (CAB), CSIC-INTA, Torrejón de Ardoz, Spain)
Journal: Geophysical Research Letters, Volume 51, Issue 11, article id. e2023GL107975.
Publication Date: Jun 2024
Origin: American Geophysical Union (AGU)
Keywords: dust deposition, dust lifting, Mars 2020, dust correction factor, solar power
Abstract Copyright: 2024. The Authors.
DOI: https://doi.org/10.1029/2023GL107975
Bibliographic Code: 2024GeoRL..5107975V
Abstract: We quantify the effect of dust accumulation at Jezero crater by means of a Dust Correction Factor (DCF) for the solar radiation measured by the photodiodes of the Radiation and Dust Sensor of the Mars 2020 mission. After one Mars Year, dust on the photodiode surface attenuated 25%-30% of the incoming solar radiation. The DCF did not decrease monotonically; we use a model to reproduce its evolution and to derive dust deposition and lifting rates, showing that dust removal is 9 times larger at Jezero crater than at InSight's location in western Elysium Planitia. The model fit obtained using observed opacities is further improved when fed with dust sedimentation rates simulated by a GCM that considers a particle size distrtibution. Projections show seasonal net dust removal, being encouraging for the long-term survival of solar-powered missions to Jezero or similarly active dust lifting regions.
Title: Inferred wind speed and direction during the descent and landing of Perseverance on Mars
Authors: Paton, M. D.; Savijärvi, H.; Harri, A.-M.; Leino, J.; Bertrand, T.; Viúdez-Moreiras, D.; Lorenz, R. D.; Newman, C.
Affiliation: AA(Finnish Meteorological Institute, PO Box 503, FIN-00101 Helsinki, Finland), AB(Finnish Meteorological Institute, PO Box 503, FIN-00101 Helsinki, Finland), AC(Finnish Meteorological Institute, PO Box 503, FIN-00101 Helsinki, Finland), AD(Finnish Meteorological Institute, PO Box 503, FIN-00101 Helsinki, Finland), AE(LESIA, Observatoire de Paris, 92195 Meudon, France), AF(Centro de Astrobiologia (CAB, CSIC-INTA) and National Institute for Aerospace Technology (INTA), Madrid, Spain), AG(Johns Hopkins University Applied Physics Laboratory, Laurel, MD, USA), AH(Aeolis Research, Chandler, AZ, USA)
Journal: Icarus, Volume 415, id.116045.
Publication Date: Jun 2024
Origin: Elsevier BV
Keywords: Mars, Wind, Atmosphere, Perseverance, Heat shield
Abstract Copyright: © 2024 Elsevier Inc. All rights reserved.
DOI: https://doi.org/10.1016/j.icarus.2024.116045
Bibliographic Code: 2024Icar..41516045P
Abstract: Perseverance successfully parachuted into Jezero crater close to its western rim on a Martian spring afternoon. In situ observations of the wind conditions during the parachute and powered descent are unavailable. These observations are important for characterising the Planetary Boundary Layer (PBL) and to better constrain atmospheric conditions in Jezero crater. We infer the winds during Perseverance's parachute descent from an altitude of 12 km down to 2 km by fitting a trajectory model to the reconstructed trajectory data published by the M2020 Entry, Descent and Landing team. Below 2 km altitude we infer the winds by analysing a High Resolution Imaging Science Experiment (HiRISE) image of the landing site that was obtained about one sol after the landing. Our inferred wind speed and direction profile indicate high speed winds at an altitude of 7 km blowing from the east and at 3 km blowing from the southwest. Below an altitude of 2 km, the winds are inferred to be easterlies. The heat shield impact on the surface was observed by Perseverance's Lander Vision System Camera (LCAM). Afterwards, ejecta clouds were observed moving towards the north of the impact site. These observations, together with the orientation of the parachute canopy on the surface, suggest near-surface winds at the time were southerlies. We have inferred the wind speed and direction during Perseverance's descent that are consistent with its horizontal motion as revealed by trajectory data and HiRISE image. Comparisons with atmospheric models suggest the high speed winds could be related to topographic forcing. This study provides constraints for atmospheric modelling and advances the characterisation of winds in Jezero crater, focusing on the vertical structure of the complex wind field present in the crater.
Title: Present-day thermal and water activity environment of the Mars Sample Return collection
Authors: Zorzano, Maria-Paz; Martínez, Germán; Polkko, Jouni; Tamppari, Leslie K.; Newman, Claire; Savijärvi, Hannu; Goreva, Yulia; Viúdez-Moreiras, Daniel; Bertrand, Tanguy; Smith, Michael; Hausrath, Elisabeth M.; Siljeström, Sandra; Benison, Kathleen; Bosak, Tanja; Czaja, Andrew D.; Debaille, Vinciane; Herd, Christopher D. K.; Mayhew, Lisa; Sephton, Mark A.; Shuster, David; Simon, Justin I.; Weiss, Benjamin; Randazzo, Nicolas; Mandon, Lucia; Brown, Adrian; Hecht, Michael H.; Martínez-Frías, Jesús
Affiliation: AA(Centro de Astrobiología (CAB), CSIC-INTA, 28850, Torrejón de Ardoz, Madrid, Spain), AB(Lunar and Planetary Institute, Universities Space Research Association, Houston, TX, USA; University of Michigan, Ann Arbor, MI, USA), AC(Finnish Meteorological Institute, Helsinki, Finland), AD(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Dr., 91109, Pasadena, CA, USA), AE(Aeolis Research, Chandler, AZ, USA), AF(University of Helsinki, Helsinki, Finland), AG(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Dr., 91109, Pasadena, CA, USA), AH(Centro de Astrobiología (CAB), CSIC-INTA, 28850, Torrejón de Ardoz, Madrid, Spain), AI(Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique (LESIA), Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Univ. Paris Diderot, Sorbonne, France), AJ(NASA Goddard Space Flight Center, Greenbelt, MD, USA), AK(Department of Geoscience, University of Nevada, Las Vegas, NV, USA), AL(RISE Research Institutes of Sweden, Stockholm, Sweden), AM(West Virginia University, Morgantown, WV, USA), AN(Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA), AO(Department of Geosciences, University of Cincinnati, Cincinnati, OH, USA), AP(Laboratoire G-Time, Université Libre de Bruxelles, Brussels, Belgium), AQ(Department of Earth and Atmospheric Sciences, University of Alberta, Edmonton, Canada), AR(Department of Geological Sciences, University of Colorado Boulder, Boulder, CO, USA), AS(Department of Earth Science and Engineering, Imperial College London, London, UK), AT(University of California, Berkeley, CA, USA), AU(Center for Isotope Cosmochemistry and Geochronology, Astromaterials Research and Exploration Science, NASA Johnson Space Center, Houston, TX, USA), AV(Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA), AW(Department of Earth and Atmospheric Sciences, University of Alberta, Edmonton, Canada), AX(Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA, USA), AY(Plancius Research, Severna Park, MD, USA), AZ(MIT Haystack Observatory, 01886, Westford, MA, USA), BA(Instituto de Geociencias (CSIC-UCM, Madrid, Spain))
Journal: Scientific Reports, Volume 14, article id. 7175.
Publication Date: Mar 2024
Origin: Springer Science and Business Media LLC
Keywords: Mars sample return, Water activity, Temperature, Habitability, Jezero, Environment
DOI: https://doi.org/10.1038/s41598-024-57458-4
Bibliographic Code: 2024NatSR..14.7175Z
Abstract: The Mars Sample Return mission intends to retrieve a sealed collection of rocks, regolith, and atmosphere sampled from Jezero Crater, Mars, by the NASA Perseverance rover mission. For all life-related research, it is necessary to evaluate water availability in the samples and on Mars. Within the first Martian year, Perseverance has acquired an estimated total mass of 355 g of rocks and regolith, and 38 μmoles of Martian atmospheric gas. Using in-situ observations acquired by the Perseverance rover, we show that the present-day environmental conditions at Jezero allow for the hydration of sulfates, chlorides, and perchlorates and the occasional formation of frost as well as a diurnal atmospheric-surface water exchange of 0.5-10 g water per m<SUP>2</SUP> (assuming a well-mixed atmosphere). At night, when the temperature drops below 190 K, the surface water activity can exceed 0.5, the lowest limit for cell reproduction. During the day, when the temperature is above the cell replication limit of 245 K, water activity is less than 0.02. The environmental conditions at the surface of Jezero Crater, where these samples were acquired, are incompatible with the cell replication limits currently known on Earth.
Title: Perseverance MEDA Atmospheric Pressure Observations—Initial Results
Authors: Harri, Ari-Matti; Paton, Mark; Hieta, Maria; Polkko, Jouni; Newman, Claire; Pla-Garcia, Jorge; Leino, Joonas; Mäkinen, Terhi; Kauhanen, Janne; Jaakonaho, Iina; Sánchez-Lavega, Agustin; Hueso, Ricardo; Genzer, Maria; Lorenz, Ralph; Lemmon, Mark; Vicente-Retortillo, Alvaro; Tamppari, Leslie K.; Viudez-Moreiras, Daniel; Torre-Juarez, Manuel de la; Savijärvi, Hannu; Rodríguez-Manfredi, Javier A.; Martinez, German
Affiliation: AA(Finnish Meteorological Institute, Helsinki, Finland), AB(Finnish Meteorological Institute, Helsinki, Finland), AC(Finnish Meteorological Institute, Helsinki, Finland), AD(Finnish Meteorological Institute, Helsinki, Finland), AE(Aeolis Research, Chandler, AZ USA), AF(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AG(Finnish Meteorological Institute, Helsinki, Finland), AH(Finnish Meteorological Institute, Helsinki, Finland), AI(Finnish Meteorological Institute, Helsinki, Finland), AJ(Finnish Meteorological Institute, Helsinki, Finland), AK(UPV/EHU, Bilbao, Spain), AL(UPV/EHU, Bilbao, Spain), AM(Finnish Meteorological Institute, Helsinki, Finland), AN(Johns Hopkins Applied Physics Laboratory, Laurel, MD USA), AO(Space Science Institute, College Station, TX USA), AP(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AQ(Jet Propulsion Laboratory/California Institute of Technology, Pasadena, CA USA), AR(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AS(Jet Propulsion Laboratory/California Institute of Technology, Pasadena, CA USA), AT(Finnish Meteorological Institute, Helsinki, Finland), AU(Centro de Astrobiología (INTA-CSIC), Madrid, Spain), AV(Lunar and Planetary Institute, Houston, TX USA)
Journal: Journal of Geophysical Research: Planets, Volume 129, Issue 3, article id. e2023JE007880.
Publication Date: Mar 2024
Origin: American Geophysical Union (AGU)
Keywords: Martian atmosphere, atmospheric pressure cycle, atmospheric tidal components, pressure measurement, baroclinic and barotropic wave forms, dust devil
Abstract Copyright: 2024. The Authors.
DOI: https://doi.org/10.1029/2023JE007880
Bibliographic Code: 2024JGRE..12907880H
Abstract: The Mars2020 Perseverance Rover landed successfully on the Martian surface on the Jezero Crater floor (18.44°N, 77.45°E) at Martian solar longitude, L<SUB>s</SUB>, ∼5° in February 2021. Since then, it has produced highly valuable environmental measurements with a versatile scientific payload including the MEDA (Mars Environmental Dynamics Analyzer) suite of environmental sensors. One of the MEDA systems is the PS pressure sensor system, which weighs 40 g and has an estimated absolute accuracy of better than 3.5 Pa and a resolution of 0.13 Pa. We present initial results from the first 414 sols of Martian atmospheric surface pressure observations by the PS, whose performance was found to meet its specifications. Observed sol-averaged atmospheric pressures follow an anticipated pattern of pressure variation in the course of the advancing season and are consistent with data from other landing missions. The observed daily pressure amplitude varies by ∼2%-5 % of the sol-averaged pressure, with absolute amplitude 10-35 Pa in an approximately direct relationship with airborne dust. During a regional dust storm, which began at L<SUB>s</SUB> ∼ 135°, the daily pressure amplitude roughly doubled. The daily pressure variations were found to be remarkably sensitive to the seasonal evolution of the atmosphere. In particular, analysis of the daily pressure signature revealed diagnostic information likely related to the regional scale structure of the atmosphere. Comparison of Perseverance pressure observations with data from other landers reveals the global scale seasonal behavior of Mars' atmosphere.
Title: Comparing Atmospheric Temperature Fluctuations Across Landed Missions
Authors: Mason, Emily L.; Smith, Michael D.; Richardson, Mark I.; Guzewich, Scott D.
Affiliation: AA(University of Maryland Baltimore County, Baltimore, MD USA; NASA Goddard Space Flight Center, Greenbelt, MD USA; Center for Research and Excellence in Space Science &amp; Technology II, Catonsville, MD USA), AB(NASA Goddard Space Flight Center, Greenbelt, MD USA), AC(Aeolis Research, Chandler, AZ USA), AD(NASA Goddard Space Flight Center, Greenbelt, MD USA)
Journal: Journal of Geophysical Research: Planets, Volume 129, Issue 1, article id. e2023JE007750.
Publication Date: Jan 2024
Origin: American Geophysical Union (AGU)
Keywords: Mars, atmosphere, MSL, Phoenix, Pathfinder, temperature
Abstract Copyright: 2024. American Geophysical Union. All Rights Reserved.
DOI: https://doi.org/10.1029/2023JE007750
Bibliographic Code: 2024JGRE..12907750M
Abstract: We analyze and compare atmospheric temperature data from three landed missions: Mars Science Laboratory (MSL) Curiosity rover, Phoenix lander, and Pathfinder lander. Pathfinder and Phoenix were lander missions that operated for 84 and 151 sols, respectively. MSL Curiosity is a rover that operates on the surface of Mars. It has recorded air temperature for more than five Mars Years (MY). We denoise and detrend temperature data from each mission and use those results to calculate variance in air temperature as a diagnostic for atmospheric variability at the surface. The results show a consistent seasonal pattern in MSL air temperature variance with little interannual variability outside major dust storms. The global dust storm in MY 34 was accompanied by a decrease in temperature variance and a muted response in peak MY 35 variance the following year. Phoenix (68°N, 2 m measurement height) and Pathfinder (19.7°N, 1.1 m measurement height) air temperatures have larger variance than air temperature from environmental data records at the MSL location (5.4°S, 1.6 m measurement height) at its equatorial latitude. Pathfinder variances per sol are larger than those of Phoenix, possibly due to a combination of Pathfinder's lower albedo surface and lower latitude. This occurs despite the Pathfinder location's higher thermal inertia, which would act to decrease noontime variance relative to a lower thermal inertia surface. Comparison of MSL temperature variance to pressure drops related to convective vortex activity shows consistent seasonal patterns; however, pressure drops tend to increase with increasing rover elevation, while variance remains consistent.
Title: Pressure Deficit in Gale Crater and a Larger Northern Polar Cap After the MY34 Global Dust Storm
Authors: de la Torre Juárez, Manuel; Piqueux, Sylvain; Kass, David M.; Newman, Claire E.; Guzewich, Scott D.
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(Aeolis Research, Pasadena, CA USA), AE(NASA Goddard Space Flight Center, Greenbelt, MD USA)
Journal: Journal of Geophysical Research: Planets, Volume 129, Issue 1, article id. e2023JE007810.
Publication Date: Jan 2024
Origin: American Geophysical Union (AGU)
Keywords: Mars science laboratory, REMS, gale, surface pressure, Mars polar cap processes, Mars general circulation
Abstract Copyright: 2024 Jet Propulsion Laboratory, California Institute of Technology. Government sponsorship acknowledged.
DOI: https://doi.org/10.1029/2023JE007810
Bibliographic Code: 2024JGRE..12907810D
Abstract: We describe the model-independent analysis technique of Mars Science Laboratory (MSL) pressure and Mars Climate Sounder (MCS) data in de la Torre Juárez et al. (2019, <A href="https://doi.org/10.22541/essoar.169945479.90436599/v1">https://doi.org/10.22541/essoar.169945479.90436599/v1</A>) that compared multiple years of surface pressures on Gale before, during, and after the Global Dust Storm of Mars Year 34. The analysis found (a) representative pressure scale heights over Gale; (b) that the storm was followed by a pressure deficit at Gale; (c) the following C storms did not eliminate the deficit; (d) changes in the duration of the polar caps condensation seasons, with an early start of the North Polar (NP) ice cap growing season the year before the Great Dust Storm (GDS) and a late signature of the end of the expansion season thereafter, changes consistent with a larger growth phase of the NP cap; (e) MCS observed a larger than usual NP cap; and (f) cold temperature anomalies over the NP and warm over the Southern Pole after the storm. We also show that the analysis of observed MSL pressure data alone filters out effects on the pressure signal that are attributable to dynamical and orographic processes in a recent model analysis that makes similar interpretations as our 2019 study. One additional Mars year of observations is included to eliminate early concerns about sensor drifts. Noting that a similar NP anomaly was observed with MCS data after the last early GDS in MY25, and not the later GDS of MY27, the results suggest a possible unique effect of early GDSs.