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1. Twin Worlds, Divergent Fates: How Obliquity has differently shaped Pluto's and Triton's landscapes and climates

Author

Bertrand, Tanguy, Forget, François, and Lellouch, Emmanuel

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Triton and Pluto are believed to share a common origin, both forming initially in the Kuiper Belt but Triton being later captured by Neptune. Both objects display similar sizes, densities, and atmospheric and surface ice composition, with the presence of volatile ices N2, CH4 and CO. Yet their appearance, including their surface albedo and ice distribution strongly differ. What can explain these different appearances? A first disparity is that Triton is experiencing significant tidal heating due to its orbit around Neptune, with subsequent resurfacing and a relatively flat surface, while Pluto is not tidally activated and displays a pronounced topography. Here we present long-term volatile transport simulations of Pluto and Triton, using the same initial conditions and volatile inventory, but with the known orbit and rotation of each object. The model reproduces, to first order, the observed volatile ice surface distribution on Pluto and Triton. Our results unambiguously demonstrate that obliquity is the main driver of the differences in surface appearance and in climate properties on Pluto and Triton, and give further support to the hypothesis that both objects had a common origin followed by a different dynamical history., Comment: 16 pages, 3 figures

Published
2024
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2. Drying of the Martian mesosphere during aphelion induced by lower temperatures

Author

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, and Rodriguez-Manfredi, Jose Antonio

Published
2024
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3. Present-day thermal and water activity environment of the Mars Sample Return collection

Author

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., and Martínez-Frías, Jesús

Published
2024
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4. Impact of the coagulation of dust particles on Mars during the 2018 global dust storm

Author

Bertrand, Tanguy, Kahre, Melinda, Urata, Richard, Määttänen, Anni, Montmessin, Franck, Wilson, John, and Wolff, Mike

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Coagulation of particles occurs when two particles collide and stick together. In the Martian atmosphere, dust coagulation would increase the effective particle size, as small particles accrete to larger particles. Murphy et al. (1990) showed that Brownian coagulation of dust in the Martian atmosphere was not significant, due to the low dust particle mixing ratios, while Montmessin et al. (2002) and Fedorova et al. (2014) showed that it mostly involves particle radii smaller than 0.1 um. However, the effects of coagulation have never been explored in 3D, during a global dust storm, i.e. in presence of larger numbers of small particles. Here we revisit this issue by using the NASA Ames Mars Global Climate Model (MGCM) to investigate the temporal and spatial changes in dust particle sizes during the 2018 global storm due to coagulation and the overall impact of these processes on Mars' climate. Our parameterization for coagulation includes the effect of Brownian motion, Brownian diffusion enhancement, and gravitational collection. We show that Brownian motion and Brownian diffusion enhancement dominate gravitational collection. The impact of coagulation is significant during the storm, with coagulation rates increased by a factor of 10 compared to non-storm conditions. The effective particle radius can be increased by a factor of 2 due to coagulation, leading to a 20K colder atmosphere above 30 km altitude. Overall, our parameterization improves the representation of the decay phase of the storm relative to observations. The process remains significant outside the storm period if large numbers of submicron-sized particles are involved. It may be possible, in GCMs, to lift larger amounts of submicron-sized particles from the surface without excess dust buildup in the atmosphere, thus improving the agreement with some of the observations without diverging from the observed column opacities., Comment: Accepted in Icarus

Published
2022
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5. Large-scale cryovolcanic resurfacing on Pluto

Author

Singer, Kelsi N., White, Oliver L., Schmitt, Bernard, Rader, Erika L., Protopapa, Silvia, Grundy, William M., Cruikshank, Dale P., Bertrand, Tanguy, Schenk, Paul M., McKinnon, William B., Stern, S. Alan, Dhingra, Rajani D., Runyon, Kirby D., Beyer, Ross A., Bray, Veronica J., Ore, Cristina Dalle, Spencer, John R., Moore, Jeffrey M., Nimmo, Francis, Keane, James T., Young, Leslie A., Olkin, Catherine B., Lauer, Tod R., Weaver, Harold A., and Ennico-Smith, Kimberly

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

The New Horizons spacecraft returned images and compositional data showing that terrains on Pluto span a variety of ages, ranging from relatively ancient, heavily cratered areas to very young surfaces with few-to-no impact craters. One of the regions with very few impact craters is dominated by enormous rises with hummocky flanks. Similar features do not exist anywhere else in the imaged solar system. Here we analyze the geomorphology and composition of the features and conclude this region was resurfaced by cryovolcanic processes, of a type and scale so far unique to Pluto. Creation of this terrain requires multiple eruption sites and a large volume of material (>104 km^3) to form what we propose are multiple, several-km-high domes, some of which merge to form more complex planforms. The existence of these massive features suggests Pluto's interior structure and evolution allows for either enhanced retention of heat or more heat overall than was anticipated before New Horizons, which permitted mobilization of water-ice-rich materials late in Pluto's history., Comment: 22 pages, including both main paper and supplement as one pdf

Published
2022
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6. The Dark Side of Pluto

Author

Lauer, Tod R., Spencer, John R., Bertrand, Tanguy, Beyer, Ross A., D, Kirby, Runyon, L, Oliver, White, Young, Leslie A., Ennico, Kimberly, McKinnon, William B., Moore, Jeffrey M., Olkin, Catherine B., Stern, S. Alan, and Weaver, Harold A.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

During its departure from Pluto, New Horizons used its LORRI camera to image a portion of Pluto's southern hemisphere that was in a decades-long seasonal winter darkness, but still very faintly illuminated by sunlight reflected by Charon. Recovery of this faint signal was technically challenging. The bright ring of sunlight forward-scattered by haze in the Plutonian atmosphere encircling the nightside hemisphere was severely overexposed, defeating the standard smeared-charge removal required for LORRI images. Reconstruction of the overexposed portions of the raw images, however, allowed adequate corrections to be accomplished. The small solar elongation of Pluto during the departure phase also generated a complex scattered-sunlight background in the images that was three orders of magnitude stronger than the estimated Charon-light flux (the Charon-light flux is similar to the flux of moonlight on Earth a few days before first quarter). A model background image was constructed for each Pluto image based on principal component analysis (PCA) applied to an ensemble of scattered-sunlight images taken at identical Sun-spacecraft geometry to the Pluto images. The recovered Charon-light image revealed a high-albedo region in the southern hemisphere. We argue that this may be a regional deposit of N_2 or CH_4 ice. The Charon-light image also shows that the south polar region currently has markedly lower albedo than the north polar region of Pluto, which may reflect the sublimation of N_2 ice or the deposition of haze particulates during the recent southern summer., Comment: 24 pages, 10 figures, published in the Planetary Science Journal

Published
2021

7. Morphological Comparison of Blocks in Chaos Terrains on Pluto, Europa, and Mars

Author

Skjetne, Helle L., Singer, Kelsi N., Hynek, Brian M., Knight, Katie I., Schenk, Paul M., Olkin, Cathy B., White, Oliver L., Bertrand, Tanguy, Runyon, Kirby D., McKinnon, William B., Moore, Jeffrey M., Stern, S. Alan, Weaver, Harold A., Young, Leslie A., and Ennico, Kim

Subjects
Astrophysics - Earth and Planetary Astrophysics, Physics - Geophysics
Abstract

Chaos terrains are characterized by disruption of preexisting surfaces into irregularly arranged mountain blocks with a chaotic appearance. Several models for chaos formation have been proposed, but the formation and evolution of this enigmatic terrain type has not yet been fully constrained. We provide extensive mapping of the individual blocks that make up different chaos landscapes, and present a morphological comparison of chaotic terrains found on Pluto, Jupiter's moon Europa, and Mars, using measurements of diameter, height, and axial ratio of chaotic mountain blocks. Additionally, we compare mountain blocks in chaotic terrain and fretted terrain on Mars. We find a positive linear relationship between the size and height of chaos blocks on Pluto and Mars, whereas blocks on Europa exhibit a flat trend as block height does not generally increase with increasing block size. Block heights on Pluto are used to estimate the block root depths if they were floating icebergs. Block heights on Europa are used to infer the total thickness of the icy layer from which the blocks formed. Finally, block heights on Mars are compared to potential layer thicknesses of near-surface material. We propose that the heights of chaotic mountain blocks on Pluto, Europa, and Mars can be used to infer information about crustal lithology and surface layer thickness., Comment: 45 pages, 3 tables, 9 figures, 5 appendices

Published
2021
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8. Global Climate Model Occultation Lightcurves Tested by August 2018 Ground-Based Stellar Occultation

Author

Chen, Sihe, Young, Eliot F., Young, Leslie A., Bertrand, Tanguy, Forget, François, and Yung, Yuk L.

Subjects
Astrophysics - Earth and Planetary Astrophysics, Physics - Atmospheric and Oceanic Physics
Abstract

Pluto's atmospheric profiles (temperature and pressure) have been studied for decades from stellar occultation lightcurves. In this paper, we look at recent Pluto Global Climate Model (GCM) results (3D temperature, pressure, and density fields) from Bertrand et al. (2020) and use the results to generate model observer's plane intensity fields (OPIF) and lightcurves by using a Fourier optics scheme to model light passing through Pluto's atmosphere (Young, 2012). This approach can accommodate arbitrary atmospheric structures and 3D distributions of haze. We compared the GCM model lightcurves with the lightcurves observed during the 15-AUG-2018 Pluto stellar occultation. We find that the climate scenario which best reproduces the observed data includes an N2 ice mid-latitude band in the southern hemisphere. We have also studied different haze and P/T ratio profiles: the haze effectively reduces the central flash strength, and a lower P/T ratio both reduces the central flash strength and incurs anomalies in the shoulders of the central flash.

Published
2021
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9. Large-scale cryovolcanic resurfacing on Pluto

Author

Singer, Kelsi N, White, Oliver L, Schmitt, Bernard, Rader, Erika L, Protopapa, Silvia, Grundy, William M, Cruikshank, Dale P, Bertrand, Tanguy, Schenk, Paul M, McKinnon, William B, Stern, S Alan, Dhingra, Rajani D, Runyon, Kirby D, Beyer, Ross A, Bray, Veronica J, Ore, Cristina Dalle, Spencer, John R, Moore, Jeffrey M, Nimmo, Francis, Keane, James T, Young, Leslie A, Olkin, Catherine B, Lauer, Tod R, Weaver, Harold A, and Ennico-Smith, Kimberly

Subjects
Earth Sciences, Physical Sciences, Space Sciences, Geology
Abstract

The New Horizons spacecraft returned images and compositional data showing that terrains on Pluto span a variety of ages, ranging from relatively ancient, heavily cratered areas to very young surfaces with few-to-no impact craters. One of the regions with very few impact craters is dominated by enormous rises with hummocky flanks. Similar features do not exist anywhere else in the imaged solar system. Here we analyze the geomorphology and composition of the features and conclude this region was resurfaced by cryovolcanic processes, of a type and scale so far unique to Pluto. Creation of this terrain requires multiple eruption sites and a large volume of material (>104 km3) to form what we propose are multiple, several-km-high domes, some of which merge to form more complex planforms. The existence of these massive features suggests Pluto's interior structure and evolution allows for either enhanced retention of heat or more heat overall than was anticipated before New Horizons, which permitted mobilization of water-ice-rich materials late in Pluto's history.

Published
2022

10. Formation, Composition, and History of the Pluto System: A Post-New-Horizons Synthesis

Author

McKinnon, William B., Glein, Christopher R., Bertrand, Tanguy, and Rhoden, Alyssa R.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

The Pluto-Charon system provides a broad variety of constraints on planetary formation, composition, chemistry, and evolution. Pluto was the first body to be discovered in what is now known as the Kuiper belt, its orbit ultimately becoming a major clue that the giant planets underwent substantial orbital migration early in Solar System history. This migration has been linked to an early instability in the orbits of the giant planets and the formation of the Kuiper belt itself, from an ancestral trans-Neptunian planetesimal disk that included Pluto. Pluto-Charon is emblematic of what are now recognized as small or dwarf planets. Far from being a cold, dead, battered icy relic, Pluto displays evidence of a complex geological history, with ongoing processes including tectonism, cryovolcanism, solid-state convection, glacial flow, atmospheric circulation, surface-atmosphere volatile exchange, aeolian processes, and atmospheric photochemistry, microphysics, and haze formation. Despite Pluto's relatively modest scale, the combination of original accretional heat, long-term internal radiogenic heat release, and external solar forcing, when combined with sufficiently volatile (and thus mobile) materials, yields an active world. Pluto may have inherited a large organic mass fraction during accretion, which may responsible, in part, for its surface and atmospheric volatiles. Charon, Pluto's major moon, displays evidence of extensive early tectonism and cryovolcanism. Dwarf planets are thus truly planetary in terms of satellite systems and geological and atmospheric complexity (if not ongoing activity). What they may lack in mass is made up in number, and the majority of the Solar System's dwarf planets remain undiscovered., Comment: 94 pages, 13 figures; will appear as a chapter/conference proceedings in the Space Science Series volume "The Pluto System After New Horizons," S.A. Stern et al., University of Arizona Press, Tucson, AZ

Published
2020
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11. Simulation of the 2018 Global Dust Storm on Mars Using the NASA Ames Mars GCM: A Multi-Tracer Approach

Author

Bertrand, Tanguy, Wilson, R. John, Kahre, Melinda A., Urata, Richard, and Kling, Alex

Subjects
Astrophysics - Earth and Planetary Astrophysics, Physics - Atmospheric and Oceanic Physics
Abstract

Global dust storms are the most thermodynamically significant dust events on Mars. They are produced from the combination of multiple local and regional lifting events and maintained by positive radiative-dynamic feedbacks. The most recent of these events, which began in June 2018, was monitored by several spacecraft in orbit and on the surface, but many questions remain regarding its onset, expansion and decay. We model the 2018 global dust storm with the NASA Ames Mars Global Climate Model to better understand the evolution of the storm and how the general circulation and finite surface dust reservoirs impact it. The global dust storm is characterized by the rapid eastward transport of dust in the equatorial regions and subsequent lifting. We highlight the rapid transfer of dust between western and eastern hemispheres reservoirs, which may play an important role in the storm development through the replenishment of surface dust. Both the Hadley cell circulation and the diurnal cycle of atmospheric heating increase in intensity with increasing dustiness. Large dust plumes are predicted during the mature stage of the storm, injecting dust up to 80 km. The water ice cloud condensation level migrates to higher altitudes, leading to the enrichment of water vapor in the upper atmosphere. In our simulations, the intensity of the Hadley cell is significantly stronger than that of non-dusty conditions. This feedback is strongly sensitive to the radiative properties of dust, which depends on the effective size of the lifted dust distribution., Comment: 40 pages, 16 figures, submitted to JGR planets

Published
2019
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12. 3D modeling of organic haze in Pluto's atmosphere

Author

Bertrand, Tanguy and Forget, François

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

The New Horizons spacecraft, which flew by Pluto on July 14, 2015, revealed the presence of haze in Pluto's atmosphere that were formed by CH4/N2 photochemistry at high altitudes in Pluto's atmosphere, as on Titan and Triton. In order to help the analysis of the observations and further investigate the formation of organic haze and its evolution at global scales, we have implemented a simple parametrization of the formation of organic haze in our Pluto General Circulation Model. The production of haze in our model is based on the different steps of aerosol formation as understood on Titan and Triton: photolysis of CH4 in the upper atmosphere by Lyman-alpha UV radiation, production of various gaseous species, and conversion into solid particles through accumulation and aggregation processes. We compared two reference simulations ran with a particle radius of 50 nm: with, and without South Pole N2 condensation. We discuss the impact of the particle radius and the lifetime of the precursors on the haze distribution. We simulate CH4 photolysis and the haze formation up to 600 km above the surface. Results show that CH4 photolysis in Pluto's atmosphere in 2015 occured mostly in the sunlit summer hemisphere with a peak at an altitude of 250 km, though the interplanetary source of Lyman-alpha flux can induce some photolysis even in the Winter hemisphere. We obtained an extensive haze up to altitudes comparable with the observations, and with non-negligible densities up to 500 km altitude. In both reference simulations, the haze density is not strongly impacted by the meridional circulation. With no South Pole N2 condensation, the maximum nadir opacity and haze extent is obtained at the North Pole. With South Pole N2 condensation, the descending parcel of air above the South Pole leads to a latitudinally more homogeneous haze density with a slight density peak at the South Pole.

Published
2017
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13. Radiation-induced alteration of apatite on the surface of Mars:first in situ observations with SuperCam Raman onboard Perseverance

Author

Clavé, E., Beyssac, O., Bernard, S., Royer, C., Lopez-Reyes, G., Schröder, S., Rammelkamp, K., Forni, O., Fau, A., Cousin, A., Manrique, J. A., Ollila, A., Madariaga, J. M., Aramendia, J., Sharma, S. K., Fornaro, T., Maurice, S., Wiens, R. C., Acosta-Maeda, Tayro, Agard, Christophe, Alberquilla, Fernando, Alvarez Llamas, Cesar, Anderson, Ryan, Applin, Daniel, Aramendia, Julene, Arana, Gorka, Beal, Roberta, Beck, Pierre, Bedford, Candice, Benzerara, Karim, Bernard, Sylvain, Bernardi, Pernelle, Bertrand, Tanguy, Beyssac, Olivier, Bloch, Thierry, Bonnet, Jean-Yves, Bousquet, Bruno, Boustelitane, Abderrahmane, Bouyssou Mann, Magali, Brand, Matthew, Cais, Philippe, Caravaca, Gwenael, De Pinedo, Kepa Castro Ortiz, Cazalla, Charlene, Charpentier, Antoine, Chide, Baptiste, Clavé, Elise, Clegg, Samuel, Cloutis, Ed, Coloma, Leire, Comellas, Jade, Connell, Stephanie, Cousin, Agnes, DeFlores, Lauren, Dehouck, Erwin, Delapp, Dot, Perez, Tomas Delgado, Deron, Robin, Donny, Christophe, Doressoundiram, Alain, Dromart, Gilles, Essunfeld, Ari, Fabre, Cecile, Fau, Amaury, Fischer, Woodward, Follic, Hugo, Forni, Olivier, Fouchet, Thierry, Francis, Raymond, Frydenvang, Jens, Gabriel, Travis, Gallegos, Zachary, García-Florentino, Cristina, Gasda, Patrick, Gasnault, Olivier, Gibbons, Erin, Gillier, Martin, Gomez, Laura, Gonzalez, Sofia, Grotzinger, John, Huidobro, Jennifer, Jacob, Xavier, Johnson, Jeffrey, Kalucha, Hemani, Kelly, Evan, Knutsen, Elise, Lacombe, Gaetan, Lamarque, Florentin, Lanza, Nina, Larmat, Carene, Laserna, Javier, Lasue, Jeremie, Le Deit, Laetitia, Le Mouelic, Stephane, Legett, Chip, Leveille, Richard, Lewin, Eric, Little, Cynthia, Loche, Mattéo, Lopez Reyes, Guillermo, Lorenz, Ralph, Lorigny, Eric, Madariaga, Juan Manuel, Madsen, Morten, Mandon, Lucia, Manelski, Henry, Mangold, Nicolas, Martinez, Jose Manrique, Martin, Noah, Martinez Frias, Jesus, Maurice, Sylvestre, Mcconnochie, Timothy, McLennan, Scott, Melikechi, Noureddine, Meslin, Pierre Yves, Meunier, Frederique, Mimoun, David, Montagnac, Gilles, Montmessin, Franck, Moros, Javier, Mousset, Valerie, Murdoch, Naomi, Nelson, Tony, Newell, Ray, Nicolas, Cécile, Newsom, Horton, O’Shea, Colleen, Ollila, Ann, Pantalacci, Philippe, Parmentier, Jonathan, Peret, Laurent, Perrachon, Pascal, Pilleri, Paolo, Pilorget, Cédric, Pinet, Patrick, Poblacion, Iratxe, Poulet, Francois, Quantin Nataf, Cathy, Rapin, William, Reyes, Ivan, Rigaud, Laurent, Robinson, Scott, Rochas, Ludovic, Root, Margaret, Ropert, Eloise, Rouverand, Léa, Royer, Clement, Perez, Fernando Rull, Said, David, Sans-Jofre, Pierre, Schroeder, Susanne, Seel, Fabian, Sharma, Shiv, Sheridan, Amanda, Sobron Sanchez, Pablo, Stcherbinine, Aurélien, Stott, Alex, Toplis, Michael, Turenne, Nathalie, Veneranda, Marco, Venhaus, Dawn, Wiens, Roger, Wolf, Uriah, Zastrow, Allison, Clavé, E., Beyssac, O., Bernard, S., Royer, C., Lopez-Reyes, G., Schröder, S., Rammelkamp, K., Forni, O., Fau, A., Cousin, A., Manrique, J. A., Ollila, A., Madariaga, J. M., Aramendia, J., Sharma, S. K., Fornaro, T., Maurice, S., Wiens, R. C., Acosta-Maeda, Tayro, Agard, Christophe, Alberquilla, Fernando, Alvarez Llamas, Cesar, Anderson, Ryan, Applin, Daniel, Aramendia, Julene, Arana, Gorka, Beal, Roberta, Beck, Pierre, Bedford, Candice, Benzerara, Karim, Bernard, Sylvain, Bernardi, Pernelle, Bertrand, Tanguy, Beyssac, Olivier, Bloch, Thierry, Bonnet, Jean-Yves, Bousquet, Bruno, Boustelitane, Abderrahmane, Bouyssou Mann, Magali, Brand, Matthew, Cais, Philippe, Caravaca, Gwenael, De Pinedo, Kepa Castro Ortiz, Cazalla, Charlene, Charpentier, Antoine, Chide, Baptiste, Clavé, Elise, Clegg, Samuel, Cloutis, Ed, Coloma, Leire, Comellas, Jade, Connell, Stephanie, Cousin, Agnes, DeFlores, Lauren, Dehouck, Erwin, Delapp, Dot, Perez, Tomas Delgado, Deron, Robin, Donny, Christophe, Doressoundiram, Alain, Dromart, Gilles, Essunfeld, Ari, Fabre, Cecile, Fau, Amaury, Fischer, Woodward, Follic, Hugo, Forni, Olivier, Fouchet, Thierry, Francis, Raymond, Frydenvang, Jens, Gabriel, Travis, Gallegos, Zachary, García-Florentino, Cristina, Gasda, Patrick, Gasnault, Olivier, Gibbons, Erin, Gillier, Martin, Gomez, Laura, Gonzalez, Sofia, Grotzinger, John, Huidobro, Jennifer, Jacob, Xavier, Johnson, Jeffrey, Kalucha, Hemani, Kelly, Evan, Knutsen, Elise, Lacombe, Gaetan, Lamarque, Florentin, Lanza, Nina, Larmat, Carene, Laserna, Javier, Lasue, Jeremie, Le Deit, Laetitia, Le Mouelic, Stephane, Legett, Chip, Leveille, Richard, Lewin, Eric, Little, Cynthia, Loche, Mattéo, Lopez Reyes, Guillermo, Lorenz, Ralph, Lorigny, Eric, Madariaga, Juan Manuel, Madsen, Morten, Mandon, Lucia, Manelski, Henry, Mangold, Nicolas, Martinez, Jose Manrique, Martin, Noah, Martinez Frias, Jesus, Maurice, Sylvestre, Mcconnochie, Timothy, McLennan, Scott, Melikechi, Noureddine, Meslin, Pierre Yves, Meunier, Frederique, Mimoun, David, Montagnac, Gilles, Montmessin, Franck, Moros, Javier, Mousset, Valerie, Murdoch, Naomi, Nelson, Tony, Newell, Ray, Nicolas, Cécile, Newsom, Horton, O’Shea, Colleen, Ollila, Ann, Pantalacci, Philippe, Parmentier, Jonathan, Peret, Laurent, Perrachon, Pascal, Pilleri, Paolo, Pilorget, Cédric, Pinet, Patrick, Poblacion, Iratxe, Poulet, Francois, Quantin Nataf, Cathy, Rapin, William, Reyes, Ivan, Rigaud, Laurent, Robinson, Scott, Rochas, Ludovic, Root, Margaret, Ropert, Eloise, Rouverand, Léa, Royer, Clement, Perez, Fernando Rull, Said, David, Sans-Jofre, Pierre, Schroeder, Susanne, Seel, Fabian, Sharma, Shiv, Sheridan, Amanda, Sobron Sanchez, Pablo, Stcherbinine, Aurélien, Stott, Alex, Toplis, Michael, Turenne, Nathalie, Veneranda, Marco, Venhaus, Dawn, Wiens, Roger, Wolf, Uriah, and Zastrow, Allison

Abstract

Planetary exploration relies considerably on mineral characterization to advance our understanding of the solar system, the planets and their evolution. Thus, we must understand past and present processes that can alter materials exposed on the surface, affecting space mission data. Here, we analyze the first dataset monitoring the evolution of a known mineral target in situ on the Martian surface, brought there as a SuperCam calibration target onboard the Perseverance rover. We used Raman spectroscopy to monitor the crystalline state of a synthetic apatite sample over the first 950 Martian days (sols) of the Mars2020 mission. We note significant variations in the Raman spectra acquired on this target, specifically a decrease in the relative contribution of the Raman signal to the total signal. These observations are consistent with the results of a UV-irradiation test performed in the laboratory under conditions mimicking ambient Martian conditions. We conclude that the observed evolution reflects an alteration of the material, specifically the creation of electronic defects, due to its exposure to the Martian environment and, in particular, UV irradiation. This ongoing process of alteration of the Martian surface needs to be taken into account for mineralogical space mission data analysis.

Published
2024

14. An acoustic investigation of the near-surface turbulence on Mars

Author

Chide, Baptiste, primary, Blanc-Benon, Philippe, additional, Bertrand, Tanguy, additional, Jacob, Xavier, additional, Lasue, Jérémie, additional, Lorenz, Ralph D., additional, Montmessin, Franck, additional, Murdoch, Naomi, additional, Pla-Garcia, Jorge, additional, Seel, Fabian, additional, Schröder, Susanne, additional, Stott, Alexander E., additional, de la Torre Juarez, Manuel, additional, and Wiens, Roger C., additional

Published
2024
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16. Nocturnal Turbulence at Jezero Crater as Determined From MEDA Measurements and Modeling

Author

Física aplicada I, Fisika aplikatua I, Plá García, Jorge, Munguira Ruiz, Asier, Rafkin, Scot, Newman, Claire E., Bertrand, Tanguy, Martínez, Germán, Hueso Alonso, Ricardo, Sánchez Lavega, Agustín María, Del Río Gaztelurrutia, María Teresa, Stott, Alexander E., Murdoch, Naomi, de la Torre Juárez, Manuel, Lemmon, Mark T., Chide, Baptiste, Viúdez Moreiras, Daniel, Savijärvi, Hannu, Richardson, Mark I., Marín Jiménez, Mercedes, Sebastián, Eduardo, Lepinette, Alain, Mora Sotomayor, Luis, Rodríguez Manfredi, José Antonio, Física aplicada I, Fisika aplikatua I, Plá García, Jorge, Munguira Ruiz, Asier, Rafkin, Scot, Newman, Claire E., Bertrand, Tanguy, Martínez, Germán, Hueso Alonso, Ricardo, Sánchez Lavega, Agustín María, Del Río Gaztelurrutia, María Teresa, Stott, Alexander E., Murdoch, Naomi, de la Torre Juárez, Manuel, Lemmon, Mark T., Chide, Baptiste, Viúdez Moreiras, Daniel, Savijärvi, Hannu, Richardson, Mark I., Marín Jiménez, Mercedes, Sebastián, Eduardo, Lepinette, Alain, Mora Sotomayor, Luis, and Rodríguez Manfredi, José Antonio

Abstract

Mars 2020 Mars Environmental Dynamics Analyzer (MEDA) instrument data acquired during half of a Martian year (Ls 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.

Published
2023

17. Mars 2020 Perseverance Rover Studies of the Martian Atmosphere Over Jezero From Pressure Measurements

Author

Física aplicada I, Fisika aplikatua I, Sánchez Lavega, Agustín María, Del Río Gaztelurrutia, María Teresa, Hueso Alonso, Ricardo, de la Torre Juárez, Manuel, Martínez, Germán M., Harri, Ari Matti, Genzer, Maria, Hieta, Maria, Polkko, J., Rodríguez Manfredi, José Antonio, Lemmon, Mark T., Plá García, Jorge, Toledo, Daniel, Vicente Retortillo, Álvaro, Viúdez Moreiras, Daniel, Munguira Ruiz, Asier, Tamppari, Leslie, Newman, Claire E., Gómez Elvira, Javier, Guzewich, Scott, Bertrand, Tanguy, Apestigue, Victor, Arruego, Ignacio, Wolff, Michael J., Banfield, Don, Jaakonaho, I., Makinen, T., Física aplicada I, Fisika aplikatua I, Sánchez Lavega, Agustín María, Del Río Gaztelurrutia, María Teresa, Hueso Alonso, Ricardo, de la Torre Juárez, Manuel, Martínez, Germán M., Harri, Ari Matti, Genzer, Maria, Hieta, Maria, Polkko, J., Rodríguez Manfredi, José Antonio, Lemmon, Mark T., Plá García, Jorge, Toledo, Daniel, Vicente Retortillo, Álvaro, Viúdez Moreiras, Daniel, Munguira Ruiz, Asier, Tamppari, Leslie, Newman, Claire E., Gómez Elvira, Javier, Guzewich, Scott, Bertrand, Tanguy, Apestigue, Victor, Arruego, Ignacio, Wolff, Michael J., Banfield, Don, Jaakonaho, I., and Makinen, T.

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 Ls ∼ 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 CO2 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 Ls ∼ 155°.

Published
2023

18. Near Surface Atmospheric Temperatures at Jezero From Mars 2020 MEDA Measurements

Author

Física aplicada I, Fisika aplikatua I, Munguira Ruiz, Asier, Hueso Alonso, Ricardo, Sánchez Lavega, Agustín María, de la Torre Juárez, Manuel, Martínez, Germán M., Newman, Claire E., Sebastián, Eduardo, Lepinette, Alain, Vicente Retortillo, Álvaro, Chide, Baptiste, Lemmon, Mark T., Bertrand, Tanguy, Lorenz, Ralph D., Banfield, Don, Gómez Elvira, Javier, Martín Soler, J., Navarro, Sara, Plá García, Jorge, Rodríguez Manfredi, José Antonio, Romeral, J., Smith, Michael D., Torres, J., Física aplicada I, Fisika aplikatua I, Munguira Ruiz, Asier, Hueso Alonso, Ricardo, Sánchez Lavega, Agustín María, de la Torre Juárez, Manuel, Martínez, Germán M., Newman, Claire E., Sebastián, Eduardo, Lepinette, Alain, Vicente Retortillo, Álvaro, Chide, Baptiste, Lemmon, Mark T., Bertrand, Tanguy, Lorenz, Ralph D., Banfield, Don, Gómez Elvira, Javier, Martín Soler, J., Navarro, Sara, Plá García, Jorge, Rodríguez Manfredi, José Antonio, Romeral, J., Smith, Michael D., and Torres, J.

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 LS = 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 LS = 153°–156° that simultaneously warmed the near surface atmosphere while cooling the surface.

Published
2023

19. Acoustic recording of near-surface turbulence on Mars

Author

Maurice, Sylvestre, primary, Blanc-Benon, Philippe, additional, Chide, Baptiste, additional, Bertrand, Tanguy, additional, Murdoch, Naomi, additional, Lorenz, Ralph, additional, Jacob, Xavier, additional, Dragna, Didier, additional, Stott, Alexander, additional, Gillier, Martin, additional, De la Torre Juarez, Manuel, additional, Rodriguez Manfredi, Jose Antonio, additional, Mimoun, David, additional, and Wiens, Roger, additional

Published
2023
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21. Martian Wind and turbulence heard by the SuperCam microphone on the perseverance rover

Author

Stott, Alexander, primary, Murdoch, Naomi, additional, Gillier, Martin, additional, Banfield, Don, additional, Bertrand, Tanguy, additional, Chide, Baptiste, additional, De la Torre Juarez, Manuel, additional, Hueso, Ricardo, additional, Lorenz, Ralph, additional, Martinez, German, additional, Munguira, Asier, additional, Mora Sotomayor, Luis, additional, Navarro, Sara, additional, Newman, Claire, additional, Pilleri, Paolo, additional, Pla-Garcia, Jorge, additional, Randazzo, Nicolas, additional, Rodriguez Manfredi, Jose Antonio, additional, Sanchez-Lavega, Agustin, additional, Smith, Michael, additional, Viudez Moreiras, Daniel, additional, Williams, Nathan, additional, Maurice, Sylvestre, additional, Wiens, Roger, additional, and Mimoun, David, additional

Published
2023
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22. Geological, multispectral, and meteorological imaging results from the Mars 2020 Perseverance rover in Jezero crater

Author

Bell, James F., primary, Maki, Justin N., additional, Alwmark, Sanna, additional, Ehlmann, Bethany L., additional, Fagents, Sarah A., additional, Grotzinger, John P., additional, Gupta, Sanjeev, additional, Hayes, Alexander, additional, Herkenhoff, Ken E., additional, Horgan, Briony H. N., additional, Johnson, Jeffrey R., additional, Kinch, Kjartan B., additional, Lemmon, Mark T., additional, Madsen, Morten B., additional, Núñez, Jorge I., additional, Paar, Gerhard, additional, Rice, Melissa, additional, Rice, James W., additional, Schmitz, Nicole, additional, Sullivan, Robert, additional, Vaughan, Alicia, additional, Wolff, Mike J., additional, Bechtold, Andreas, additional, Bosak, Tanja, additional, Duflot, Louise E., additional, Fairén, Alberto G., additional, Garczynski, Brad, additional, Jaumann, Ralf, additional, Merusi, Marco, additional, Million, Chase, additional, Ravanis, Eleni, additional, Shuster, David L., additional, Simon, Justin, additional, St. Clair, Michael, additional, Tate, Christian, additional, Walter, Sebastian, additional, Weiss, Benjamin, additional, Bailey, Alyssa M., additional, Bertrand, Tanguy, additional, Beyssac, Olivier, additional, Brown, Adrian J., additional, Caballo-Perucha, Piluca, additional, Caplinger, Michael A., additional, Caudill, Christy M., additional, Cary, Francesca, additional, Cisneros, Ernest, additional, Cloutis, Edward A., additional, Cluff, Nathan, additional, Corlies, Paul, additional, Crawford, Kelsie, additional, Curtis, Sabrina, additional, Deen, Robert, additional, Dixon, Darian, additional, Donaldson, Christopher, additional, Barrington, Megan, additional, Ficht, Michelle, additional, Fleron, Stephanie, additional, Hansen, Michael, additional, Harker, David, additional, Howson, Rachel, additional, Huggett, Joshua, additional, Jacob, Samantha, additional, Jensen, Elsa, additional, Jensen, Ole B., additional, Jodhpurkar, Mohini, additional, Joseph, Jonathan, additional, Juarez, Christian, additional, Kah, Linda C., additional, Kanine, Oak, additional, Kristensen, Jessica, additional, Kubacki, Tex, additional, Lapo, Kristiana, additional, Magee, Angela, additional, Maimone, Michael, additional, Mehall, Greg L., additional, Mehall, Laura, additional, Mollerup, Jess, additional, Viúdez-Moreiras, Daniel, additional, Paris, Kristen, additional, Powell, Kathryn E., additional, Preusker, Frank, additional, Proton, Jon, additional, Rojas, Corrine, additional, Sallurday, Danny, additional, Saxton, Kim, additional, Scheller, Eva, additional, Seeger, Christiana H., additional, Starr, Mason, additional, Stein, Nathan, additional, Turenne, Nathalie, additional, Van Beek, Jason, additional, Winhold, Andrew G., additional, and Yingling, Rachel, additional

Published
2022
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23. Acoustics Reveals Short‐Term Air Temperature Fluctuations Near Mars' Surface

Author

Chide, Baptiste, primary, Bertrand, Tanguy, additional, Lorenz, Ralph D., additional, Munguira, Asier, additional, Hueso, Ricardo, additional, Sánchez‐Lavega, Agustin, additional, Martinez, German, additional, Spiga, Aymeric, additional, Jacob, Xavier, additional, de la Torre Juarez, Manuel, additional, Lemmon, Mark T., additional, Banfield, Don, additional, Newman, Claire E., additional, Murdoch, Naomi, additional, Stott, Alexander, additional, Viúdez‐Moreiras, Daniel, additional, Pla‐Garcia, Jorge, additional, Larmat, Carène, additional, Lanza, Nina L., additional, Rodríguez‐Manfredi, José Antonio, additional, and Wiens, Roger C., additional

Published
2022
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25. EMIRS Observations of the Aphelion‐Season Mars Atmosphere

Author

Smith, Michael D., primary, Badri, Khalid, additional, Atwood, Samuel A., additional, Edwards, Christopher S., additional, Christensen, Philip R., additional, Wolff, Michael J., additional, Bertrand, Tanguy, additional, Forget, François, additional, Al Tunaiji, Eman, additional, Wolfe, Christopher, additional, Smith, Nathan, additional, and Anwar, Saadat, additional

Published
2022
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26. The dynamic atmospheric and aeolian environment of Jezero crater, Mars

Author

Newman, Claire E., primary, Hueso, Ricardo, additional, Lemmon, Mark T., additional, Munguira, Asier, additional, Vicente-Retortillo, Álvaro, additional, Apestigue, Víctor, additional, Martínez, Germán M., additional, Toledo, Daniel, additional, Sullivan, Rob, additional, Herkenhoff, Ken E., additional, de la Torre Juárez, Manuel, additional, Richardson, Mark I., additional, Stott, Alexander E., additional, Murdoch, Naomi, additional, Sanchez-Lavega, Agustín, additional, Wolff, Michael J., additional, Arruego, Ignacio, additional, Sebastián, Eduardo, additional, Navarro, Sara, additional, Gómez-Elvira, Javier, additional, Tamppari, Leslie, additional, Smith, Michael D., additional, Lepinette, Alain, additional, Viúdez-Moreiras, Daniel, additional, Harri, Ari-Matti, additional, Genzer, Maria, additional, Hieta, Maria, additional, Lorenz, Ralph D., additional, Conrad, Pan, additional, Gómez, Felipe, additional, McConnochie, Timothy H., additional, Mimoun, David, additional, Tate, Christian, additional, Bertrand, Tanguy, additional, Bell, James F., additional, Maki, Justin N., additional, Rodriguez-Manfredi, Jose Antonio, additional, Wiens, Roger C., additional, Chide, Baptiste, additional, Maurice, Sylvestre, additional, Zorzano, Maria-Paz, additional, Mora, Luis, additional, Baker, Mariah M., additional, Banfield, Don, additional, Pla-Garcia, Jorge, additional, Beyssac, Olivier, additional, Brown, Adrian, additional, Clark, Ben, additional, Montmessin, Franck, additional, Fischer, Erik, additional, Patel, Priyaben, additional, del Río-Gaztelurrutia, Teresa, additional, Fouchet, Thierry, additional, Francis, Raymond, additional, and Guzewich, Scott D., additional

Published
2022
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27. Constraints on the structure and seasonal variations of Triton's atmosphere from the 5 October 2017 stellar occultation and previous observations

Author

Marques Oliveira, Joana, Sicardy, Bruno, Gomes Júnior, Altair R., Ortiz, Jose L., Strobel, Darrell F., Bertrand, Tanguy, Forget, François, Lellouch, Emmanuel, Desmars, Josselin, Berard, Diane, Doressoundiram, Alain, Lecacheux, J., Leiva, Rodrigo, Meza, Erick, Roques, Françoise, Souami, Damya, Widemann, Thomas, Santos-Sanz, Pablo, Morales, N., Duffard, Rene, and Gallego, Sofia G.

Subjects
planets and satellites: atmospheres, techniques: photometric, planets and satellites: physical evolution, data analysis, methods: observational, techniques: photometric [methods], methods: data analysis
Abstract

Context. A stellar occultation by Neptune’s main satellite, Triton, was observed on 5 October 2017 from Europe, North Africa, and the USA. We derived 90 light curves from this event, 42 of which yielded a central flash detection. Aims. We aimed at constraining Triton’s atmospheric structure and the seasonal variations of its atmospheric pressure since the Voyager 2 epoch (1989). We also derived the shape of the lower atmosphere from central flash analysis. Methods. We used Abel inversions and direct ray-tracing code to provide the density, pressure, and temperature profiles in the altitude range ~8 km to ~190 km, corresponding to pressure levels from 9 µbar down to a few nanobars. Results. (i) A pressure of 1.18 ± 0.03 µbar is found at a reference radius of 1400 km (47 km altitude). (ii) A new analysis of the Voyager 2 radio science occultation shows that this is consistent with an extrapolation of pressure down to the surface pressure obtained in 1989. (iii) A survey of occultations obtained between 1989 and 2017 suggests that an enhancement in surface pressure as reported during the 1990s might be real, but debatable, due to very few high S/N light curves and data accessible for reanalysis. The volatile transport model analysed supports a moderate increase in surface pressure, with a maximum value around 2005-2015 no higher than 23 µbar. The pressures observed in 1995-1997 and 2017 appear mutually inconsistent with the volatile transport model presented here. (iv) The central flash structure does not show evidence of an atmospheric distortion. We find an upper limit of 0.0011 for the apparent oblateness of the atmosphere near the 8 km altitude., Astronomy & Astrophysics, 659, ISSN:0004-6361, ISSN:1432-0746

Published
2022

28. The sound of a Martian dust devil

Author

Física aplicada I, Fisika aplikatua I, Murdoch, Naomi, Stott, Alexander E., Gillier, M., Hueso Alonso, Ricardo, Lemmon, Mark T., Martínez, Germán, Apestigue, Victor, Toledo, Daniel, Lorenz, Ralph D., Chide, Baptiste, Munguira Ruiz, Asier, Sánchez Lavega, Agustín María, Vicente Retortillo, Álvaro, Newman, Claire E., Maurice, Sylvestre, de la Torre Juárez, Manuel, Bertrand, Tanguy, Banfield, Don, Navarro, Sara, Marín Jiménez, Mercedes, Torres Redondo, Josefina, Gómez Elvira, Javier, Jacob, Xavier, Cadu, A., Sournac, A., Rodríguez Manfredi, José Antonio, Wiens, Roger C., Mimoun, David, Física aplicada I, Fisika aplikatua I, Murdoch, Naomi, Stott, Alexander E., Gillier, M., Hueso Alonso, Ricardo, Lemmon, Mark T., Martínez, Germán, Apestigue, Victor, Toledo, Daniel, Lorenz, Ralph D., Chide, Baptiste, Munguira Ruiz, Asier, Sánchez Lavega, Agustín María, Vicente Retortillo, Álvaro, Newman, Claire E., Maurice, Sylvestre, de la Torre Juárez, Manuel, Bertrand, Tanguy, Banfield, Don, Navarro, Sara, Marín Jiménez, Mercedes, Torres Redondo, Josefina, Gómez Elvira, Javier, Jacob, Xavier, Cadu, A., Sournac, A., Rodríguez Manfredi, José Antonio, Wiens, Roger C., and Mimoun, David

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 25m large, at least 118m tall, and passed directly over the rover travelling at approximately 5ms-1. 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.

Published
2022

29. Geological, multispectral, and meteorological imaging results from the Mars 2020 Perseverance rover in Jezero crater

Author

Bell, James F., Maki, Justin N., Alwmark, Sanna, Ehlmann, Bethany L., Fagents, Sarah A., Grotzinger, John P., Gupta, Sanjeev, Hayes, Alexander, Herkenhoff, Ken E., Horgan, Briony H. N., Johnson, Jeffrey R., Kinch, Kjartan B., Lemmon, Mark T., Madsen, Morten B., Nunez, Jorge, Paar, Gerhard, Rice, Melissa, Rice, James W., Schmitz, Nicole, Sullivan, Robert, Vaughan, Alicia, Wolff, Mike J., Bechtold, Andreas, Bosak, Tanja, Duflot, Louise E., Fairen, Alberto G., Garczynski, Brad, Jaumann, Ralf, Merusi, Marco, Million, Chase, Ravanis, Eleni, Shuster, David L., Simon, Justin, St Clair, Michael, Tate, Christian, Walter, Sebastian, Weiss, Benjamin, Bailey, Alyssa M., Bertrand, Tanguy, Beyssac, Olivier, Brown, Adrian J., Caballo-Perucha, Piluca, Caplinger, Michael A., Caudill, Christy M., Cary, Francesca, Cisneros, Ernest, Cloutis, Edward A., Cluff, Nathan, Corlies, Paul, Crawford, Kelsie, Curtis, Sabrina, Deen, Robert, Dixon, Darian, Donaldson, Christopher, Barrington, Megan, Ficht, Michelle, Fleron, Stephanie, Hansen, Michael, Harker, David, Howson, Rachel, Huggett, Joshua, Jacob, Samantha, Jensen, Elsa, Jensen, Ole B., Jodhpurkar, Mohini, Joseph, Jonathan, Juarez, Christian, Kah, Linda C., Kanine, Oak, Kristensen, Jessica, Kubacki, Tex, Lapo, Kristiana, Magee, Angela, Maimone, Michael, Mehall, Greg L., Mehall, Laura, Mollerup, Jess, Viudez-Moreiras, Daniel, Paris, Kristen, Powell, Kathryn E., Preusker, Frank, Proton, Jon, Rojas, Corrine, Sallurday, Danny, Saxton, Kim, Scheller, Eva, Seeger, Christiana H., Starr, Mason, Stein, Nathan, Turenne, Nathalie, Van Beek, Jason, Winhold, Andrew G., Yingling, Rachel, Bell, James F., Maki, Justin N., Alwmark, Sanna, Ehlmann, Bethany L., Fagents, Sarah A., Grotzinger, John P., Gupta, Sanjeev, Hayes, Alexander, Herkenhoff, Ken E., Horgan, Briony H. N., Johnson, Jeffrey R., Kinch, Kjartan B., Lemmon, Mark T., Madsen, Morten B., Nunez, Jorge, Paar, Gerhard, Rice, Melissa, Rice, James W., Schmitz, Nicole, Sullivan, Robert, Vaughan, Alicia, Wolff, Mike J., Bechtold, Andreas, Bosak, Tanja, Duflot, Louise E., Fairen, Alberto G., Garczynski, Brad, Jaumann, Ralf, Merusi, Marco, Million, Chase, Ravanis, Eleni, Shuster, David L., Simon, Justin, St Clair, Michael, Tate, Christian, Walter, Sebastian, Weiss, Benjamin, Bailey, Alyssa M., Bertrand, Tanguy, Beyssac, Olivier, Brown, Adrian J., Caballo-Perucha, Piluca, Caplinger, Michael A., Caudill, Christy M., Cary, Francesca, Cisneros, Ernest, Cloutis, Edward A., Cluff, Nathan, Corlies, Paul, Crawford, Kelsie, Curtis, Sabrina, Deen, Robert, Dixon, Darian, Donaldson, Christopher, Barrington, Megan, Ficht, Michelle, Fleron, Stephanie, Hansen, Michael, Harker, David, Howson, Rachel, Huggett, Joshua, Jacob, Samantha, Jensen, Elsa, Jensen, Ole B., Jodhpurkar, Mohini, Joseph, Jonathan, Juarez, Christian, Kah, Linda C., Kanine, Oak, Kristensen, Jessica, Kubacki, Tex, Lapo, Kristiana, Magee, Angela, Maimone, Michael, Mehall, Greg L., Mehall, Laura, Mollerup, Jess, Viudez-Moreiras, Daniel, Paris, Kristen, Powell, Kathryn E., Preusker, Frank, Proton, Jon, Rojas, Corrine, Sallurday, Danny, Saxton, Kim, Scheller, Eva, Seeger, Christiana H., Starr, Mason, Stein, Nathan, Turenne, Nathalie, Van Beek, Jason, Winhold, Andrew G., and Yingling, Rachel

Abstract

Perseverance's Mastcam-Z instrument provides high-resolution stereo and multispectral images with a unique combination of spatial resolution, spatial coverage, and wavelength coverage along the rover's traverse in Jezero crater, Mars. Images reveal rocks consistent with an igneous (including volcanic and/or volcaniclastic) and/or impactite origin and limited aqueous alteration, including polygonally fractured rocks with weathered coatings; massive boulder-forming bedrock consisting of mafic silicates, ferric oxides, and/or iron-bearing alteration minerals; and coarsely layered outcrops dominated by olivine. Pyroxene dominates the iron-bearing mineralogy in the finegrained regolith, while olivine dominates the coarse-grained regolith. Solar and atmospheric imaging observations show significant intra- and intersol variations in dust optical depth and water ice clouds, as well as unique examples of boundary layer vortex action from both natural (dust devil) and Ingenuity helicopter-induced dust lifting. High-resolution stereo imaging also provides geologic context for rover operations, other instrument observations, and sample selection, characterization, and confirmation.

Published
2022

30. Compositionally and density stratified igneous terrain in Jezero crater, Mars

Author

Wiens, Roger C., Udry, Arya, Beyssac, Olivier, Quantin-Nataf, Cathy, Mangold, Nicolas, Cousin, Agnès, Mandon, Lucia, Bosak, Tanja, Forni, Olivier, McLennan, Scott M., Sautter, Violaine, Brown, Adrian, Benzerara, Karim, Johnson, Jeffrey R., Mayhew, Lisa, Maurice, Sylvestre, Anderson, Ryan B., Clegg, Samuel M., Crumpler, Larry, Gabriel, Travis S. J., Gasda, Patrick, Hall, James, Horgan, Briony H. N., Kah, Linda, Legett, Carey, Madariaga, Juan Manuel, Meslin, Pierre-Yves, Ollila, Ann M., Poulet, Francois, Royer, Clement, Sharma, Shiv K., Siljeström, Sandra, Simon, Justin I., Acosta-Maeda, Tayro E., Alvarez-Llamas, Cesar, Angel, S. Michael, Arana, Gorka, Beck, Pierre, Bernard, Sylvain, Bertrand, Tanguy, Bousquet, Bruno, Castro, Kepa, Chide, Baptiste, Clavé, Elise, Cloutis, Ed, Connell, Stephanie, Dehouck, Erwin, Dromart, Gilles, Fischer, Woodward, Fouchet, Thierry, Francis, Raymond, Frydenvang, Jens, Gasnault, Olivier, Gibbons, Erin, Gupta, Sanjeev, Hausrath, Elisabeth M., Jacob, Xavier, Kalucha, Hemani, Kelly, Evan, Knutsen, Elise, Lanza, Nina, Laserna, Javier, Lasue, Jeremie, Le Mouélic, Stéphane, Leveille, Richard, Lopez-Reyes, Guillermo, Lorenz, Ralph, Manrique, Jose Antonio, Martinez-Frias, Jesus, McConnochie, Tim, Melikechi, Noureddine, Mimoun, David, Montmessin, Franck, Moros, Javier, Murdoch, Naomi, Pilleri, Paolo, Pilorget, Cedric, Pinet, Patrick, Rapin, William, Rull, Fernando, Schröder, Susanne, Shuster, David L., Smith, Rebecca J., Stott, Alexander E., Tarnas, Jesse, Turenne, Nathalie, Veneranda, Marco, Vogt, David S., Weiss, Benjamin P., Willis, Peter, Stack, Kathryn M., Williford, Kenneth H., Farley, Kenneth A., Wiens, Roger C., Udry, Arya, Beyssac, Olivier, Quantin-Nataf, Cathy, Mangold, Nicolas, Cousin, Agnès, Mandon, Lucia, Bosak, Tanja, Forni, Olivier, McLennan, Scott M., Sautter, Violaine, Brown, Adrian, Benzerara, Karim, Johnson, Jeffrey R., Mayhew, Lisa, Maurice, Sylvestre, Anderson, Ryan B., Clegg, Samuel M., Crumpler, Larry, Gabriel, Travis S. J., Gasda, Patrick, Hall, James, Horgan, Briony H. N., Kah, Linda, Legett, Carey, Madariaga, Juan Manuel, Meslin, Pierre-Yves, Ollila, Ann M., Poulet, Francois, Royer, Clement, Sharma, Shiv K., Siljeström, Sandra, Simon, Justin I., Acosta-Maeda, Tayro E., Alvarez-Llamas, Cesar, Angel, S. Michael, Arana, Gorka, Beck, Pierre, Bernard, Sylvain, Bertrand, Tanguy, Bousquet, Bruno, Castro, Kepa, Chide, Baptiste, Clavé, Elise, Cloutis, Ed, Connell, Stephanie, Dehouck, Erwin, Dromart, Gilles, Fischer, Woodward, Fouchet, Thierry, Francis, Raymond, Frydenvang, Jens, Gasnault, Olivier, Gibbons, Erin, Gupta, Sanjeev, Hausrath, Elisabeth M., Jacob, Xavier, Kalucha, Hemani, Kelly, Evan, Knutsen, Elise, Lanza, Nina, Laserna, Javier, Lasue, Jeremie, Le Mouélic, Stéphane, Leveille, Richard, Lopez-Reyes, Guillermo, Lorenz, Ralph, Manrique, Jose Antonio, Martinez-Frias, Jesus, McConnochie, Tim, Melikechi, Noureddine, Mimoun, David, Montmessin, Franck, Moros, Javier, Murdoch, Naomi, Pilleri, Paolo, Pilorget, Cedric, Pinet, Patrick, Rapin, William, Rull, Fernando, Schröder, Susanne, Shuster, David L., Smith, Rebecca J., Stott, Alexander E., Tarnas, Jesse, Turenne, Nathalie, Veneranda, Marco, Vogt, David S., Weiss, Benjamin P., Willis, Peter, Stack, Kathryn M., Williford, Kenneth H., and Farley, Kenneth A.

Abstract

Before Perseverance, Jezero crater's floor was variably hypothesized to have a lacustrine, lava, volcanic airfall, or aeolian origin. SuperCam observations in the first 286 Mars days on Mars revealed a volcanic and intrusive terrain with compositional and density stratification. The dominant lithology along the traverse is basaltic, with plagioclase enrichment in stratigraphically higher locations. Stratigraphically lower, layered rocks are richer in normative pyroxene. The lowest observed unit has the highest inferred density and is olivine-rich with coarse (1.5 millimeters) euhedral, relatively unweathered grains, suggesting a cumulate origin. This is the first martian cumulate and shows similarities to martian meteorites, which also express olivine disequilibrium. Alteration materials including carbonates, sulfates, perchlorates, hydrated silicates, and iron oxides are pervasive but low in abundance, suggesting relatively brief lacustrine conditions. Orbital observations link the Jezero floor lithology to the broader Nili-Syrtis region, suggesting that density-driven compositional stratification is a regional characteristic.

Published
2022

31. Constraints on the structure and seasonal variations of Triton's atmosphere from the 5 October 2017 stellar occultation and previous observations

Author

Física aplicada I, Fisika aplikatua I, Marques Oliveira, Joana, Sicardy, Bruno, Gómes Junior, A.R., Ortiz, J.L., Strobel, D.F., Bertrand, Tanguy, Forget, F., Lellouch, E., Desmars, J., Bérard, D., Doressoundiram, A., Lecacheux, J., Leiva, R., Meza, E., Roques, F., Souami, D., Widemann, Thomas, Santos Sanz, Pablo, Morales, N., Duffard, Rene, Fernández Valenzuela, Estela, Castro Tirado, A.J., Braga Ribas, Felipe, Morgado, Bruno, Assafin, Marcelo, Bueno de Camargo, Julio Ignacio, Vieira Martins, Roberto, Benedetti Rossi, Gustavo, Santos Filho, S., Banda Huarca, M.V., Quispe Huaynasi, F., Pereira, Chrystian Luciano, Rommel, Flavia Luane, Margoti, Giuliano, Dias Oliveira, A., Colas, F., Berthier, J., Renner, S., Hueso Alonso, Ricardo, Pérez Hoyos, Santiago, Sánchez Lavega, Agustín María, Rojas Palenzuela, José Félix, Beisker, W., Kretlow, Mike, Herald, D., Gault, D., Bath, K.-L., Bode, H.-J., Bredner, E., Guhl, K., Haymes, T.V., Hummel, E., Kattentidt, B., Klös, O., Pratt, A., Thome, B., Avdellidou, Chrysa, Gazeas, K., Karampotsiou, E., Tzouganatos, L., Kardasis, E., Christou, A.A., Xilouris, Emmanuel, Alikakos, I., Gourzelas, A., Liakos, Alexios, Charmandaris, Vassilis, Jelínek, Martin, Štrobl, Jan, Eberle, A., Rapp, K., Gährken, B., Klemt, B., Kowollik, S., Bitzer, R., Miller, M., Herzogenrath, G., Frangenberg, Dirk, Brandis, L., Pütz, I., Perdelwitz, Volker, Piehler, G. M., Riepe, P., von Poschinger, K., Baruffetti, P., Cenadelli, D., Christille, J.-M., Ciabattari, F., Di Luca, R., Alboresi, D., Leto, Giuseppe, Zanmar Sánchez, R., Bruno, P., Occhipinti, G., Morrone, L., Cupolino, L., Noschese, A., Vecchione, A., Scalia, Cesare, Lo Savio, R., Giardina, G., Kamoun, S., Barbosa, R., Behrend, R., Spano, M., Bouchet, E., Cottier, M., Falco, L., G. Gallego, Sofía, Tortorelli, Luca, Sposetti, S., Sussenbach, J., Van Den Abbeel, F., André, P., Llibre, M., Pailler, Frédéric, Ardissone, J., Boutet, Michel, Sánchez, J., Bretton, M., Cailleau, A., Pic, V., Granier, L., Chauvet, R., Conjat, M., Dauvergne, J.L., Dechambre, O., Delay, P., Delcroix, Marc, Rousselot, Lionel, Ferreira, João, Machado, Pedro, Tanga, P., Rivet, J.-P., Frappa, Eric, Irzyk, M., Jabet, F., Kaschinski, M., Klotz, A., Rieugnie, Y., Klotz, A.N., Labrevoir, O., Lavandier, D., Walliang, D., Leroy, A., Bouley, S., Lisciandra, S., Coliac, Jean-François, Metz, F., Erpelding, D., Nougayrede, Jean-Philippe, Midavaine, T., Miniou, M., Moindrot, S., Morel, P., Reginato, B., Reginato, E., Rudelle, J., Tregon, B., Tanguy, R., David, J., Thuillot, W., Hestroffer, D., Vaudescal, G., Baba Aissa, D., Grigahcene, Z., Briggs, D., Broadbent, Stephen, Denyer, P., Haigh, Nicholas, Quinn, N., Thurston, G., Fossey, S. J., Arena, C., Jennings, M., talbot, J., Alonso Burgos, Sergio, Román Reche, A., Casanova, V., Briggs, E., Iglesias Marzoa, Ramón, Abril Ibáñez, J., Díaz Martín, M.C., González, H., Maestre García, J.L., Marchant, Jonathan, Ordoñez Etxeberria, Iñaki, Martorell, P., Salamero, J., Organero, F., Ana, L., Fonseca, F., Peris, V., Brevia, O., Selva, A., Perelló Pérez, Carlos, Cabedo, V., Gonçalves, Rui M. D., Ferreira, M., Marques Dias, Filipe, Daassou, A., Barkaoui, Khalid, Benkhaldoun, Z., Guennoun, M., Chouqar, J., Jehin, E., Rinner, C., Lloyd, J., El Moutamid, Maryame, Lamarche, C., Pollock, J.T., caton, D.B., Kouprianov, Vladimir, Timerson, B.W., Blanchard, G., Payet, B., Peyrot, A., Teng-Chuen-Yu, J.-P., Françoise, J., Mondon, Bernard, Payet, Thierry, Boissel, C., Castets, M., Hubbard, William, Hill, R., Reitsema, H. J., Mousis, Olivier, Ball, L., Neilsen, G., Hutcheon, S., lay, K., Anderson, P., Moy, M., Jonsen, M., Pink, I., Walters, R., Downs, B., Física aplicada I, Fisika aplikatua I, Marques Oliveira, Joana, Sicardy, Bruno, Gómes Junior, A.R., Ortiz, J.L., Strobel, D.F., Bertrand, Tanguy, Forget, F., Lellouch, E., Desmars, J., Bérard, D., Doressoundiram, A., Lecacheux, J., Leiva, R., Meza, E., Roques, F., Souami, D., Widemann, Thomas, Santos Sanz, Pablo, Morales, N., Duffard, Rene, Fernández Valenzuela, Estela, Castro Tirado, A.J., Braga Ribas, Felipe, Morgado, Bruno, Assafin, Marcelo, Bueno de Camargo, Julio Ignacio, Vieira Martins, Roberto, Benedetti Rossi, Gustavo, Santos Filho, S., Banda Huarca, M.V., Quispe Huaynasi, F., Pereira, Chrystian Luciano, Rommel, Flavia Luane, Margoti, Giuliano, Dias Oliveira, A., Colas, F., Berthier, J., Renner, S., Hueso Alonso, Ricardo, Pérez Hoyos, Santiago, Sánchez Lavega, Agustín María, Rojas Palenzuela, José Félix, Beisker, W., Kretlow, Mike, Herald, D., Gault, D., Bath, K.-L., Bode, H.-J., Bredner, E., Guhl, K., Haymes, T.V., Hummel, E., Kattentidt, B., Klös, O., Pratt, A., Thome, B., Avdellidou, Chrysa, Gazeas, K., Karampotsiou, E., Tzouganatos, L., Kardasis, E., Christou, A.A., Xilouris, Emmanuel, Alikakos, I., Gourzelas, A., Liakos, Alexios, Charmandaris, Vassilis, Jelínek, Martin, Štrobl, Jan, Eberle, A., Rapp, K., Gährken, B., Klemt, B., Kowollik, S., Bitzer, R., Miller, M., Herzogenrath, G., Frangenberg, Dirk, Brandis, L., Pütz, I., Perdelwitz, Volker, Piehler, G. M., Riepe, P., von Poschinger, K., Baruffetti, P., Cenadelli, D., Christille, J.-M., Ciabattari, F., Di Luca, R., Alboresi, D., Leto, Giuseppe, Zanmar Sánchez, R., Bruno, P., Occhipinti, G., Morrone, L., Cupolino, L., Noschese, A., Vecchione, A., Scalia, Cesare, Lo Savio, R., Giardina, G., Kamoun, S., Barbosa, R., Behrend, R., Spano, M., Bouchet, E., Cottier, M., Falco, L., G. Gallego, Sofía, Tortorelli, Luca, Sposetti, S., Sussenbach, J., Van Den Abbeel, F., André, P., Llibre, M., Pailler, Frédéric, Ardissone, J., Boutet, Michel, Sánchez, J., Bretton, M., Cailleau, A., Pic, V., Granier, L., Chauvet, R., Conjat, M., Dauvergne, J.L., Dechambre, O., Delay, P., Delcroix, Marc, Rousselot, Lionel, Ferreira, João, Machado, Pedro, Tanga, P., Rivet, J.-P., Frappa, Eric, Irzyk, M., Jabet, F., Kaschinski, M., Klotz, A., Rieugnie, Y., Klotz, A.N., Labrevoir, O., Lavandier, D., Walliang, D., Leroy, A., Bouley, S., Lisciandra, S., Coliac, Jean-François, Metz, F., Erpelding, D., Nougayrede, Jean-Philippe, Midavaine, T., Miniou, M., Moindrot, S., Morel, P., Reginato, B., Reginato, E., Rudelle, J., Tregon, B., Tanguy, R., David, J., Thuillot, W., Hestroffer, D., Vaudescal, G., Baba Aissa, D., Grigahcene, Z., Briggs, D., Broadbent, Stephen, Denyer, P., Haigh, Nicholas, Quinn, N., Thurston, G., Fossey, S. J., Arena, C., Jennings, M., talbot, J., Alonso Burgos, Sergio, Román Reche, A., Casanova, V., Briggs, E., Iglesias Marzoa, Ramón, Abril Ibáñez, J., Díaz Martín, M.C., González, H., Maestre García, J.L., Marchant, Jonathan, Ordoñez Etxeberria, Iñaki, Martorell, P., Salamero, J., Organero, F., Ana, L., Fonseca, F., Peris, V., Brevia, O., Selva, A., Perelló Pérez, Carlos, Cabedo, V., Gonçalves, Rui M. D., Ferreira, M., Marques Dias, Filipe, Daassou, A., Barkaoui, Khalid, Benkhaldoun, Z., Guennoun, M., Chouqar, J., Jehin, E., Rinner, C., Lloyd, J., El Moutamid, Maryame, Lamarche, C., Pollock, J.T., caton, D.B., Kouprianov, Vladimir, Timerson, B.W., Blanchard, G., Payet, B., Peyrot, A., Teng-Chuen-Yu, J.-P., Françoise, J., Mondon, Bernard, Payet, Thierry, Boissel, C., Castets, M., Hubbard, William, Hill, R., Reitsema, H. J., Mousis, Olivier, Ball, L., Neilsen, G., Hutcheon, S., lay, K., Anderson, P., Moy, M., Jonsen, M., Pink, I., Walters, R., and Downs, B.

Abstract

Context. A stellar occultation by Neptune's main satellite, Triton, was observed on 5 October 2017 from Europe, North Africa, and the USA. We derived 90 light curves from this event, 42 of which yielded a central flash detection. Aims. We aimed at constraining Triton's atmospheric structure and the seasonal variations of its atmospheric pressure since the Voyager 2 epoch (1989). We also derived the shape of the lower atmosphere from central flash analysis. Methods. We used Abel inversions and direct ray-tracing code to provide the density, pressure, and temperature profiles in the altitude range similar to 8 km to similar to 190 km, corresponding to pressure levels from 9 mu bar down to a few nanobars. Results. (i) A pressure of 1.18 +/- 0.03 mu bar is found at a reference radius of 1400 km (47 km altitude). (ii) A new analysis of the Voyager 2 radio science occultation shows that this is consistent with an extrapolation of pressure down to the surface pressure obtained in 1989. (iii) A survey of occultations obtained between 1989 and 2017 suggests that an enhancement in surface pressure as reported during the 1990s might be real, but debatable, due to very few high S/N light curves and data accessible for reanalysis. The volatile transport model analysed supports a moderate increase in surface pressure, with a maximum value around 2005-2015 no higher than 23 mu bar. The pressures observed in 1995-1997 and 2017 appear mutually inconsistent with the volatile transport model presented here. (iv) The central flash structure does not show evidence of an atmospheric distortion. We find an upper limit of 0.0011 for the apparent oblateness of the atmosphere near the 8 km altitude.

Published
2022

32. The dynamic atmospheric and aeolian environment of Jezero crater, Mars

Author

Física aplicada I, Fisika aplikatua I, Newman, Claire E., Hueso Alonso, Ricardo, Lemmon, Mark T., Munguira Ruiz, Asier, Vicente Retortillo, Álvaro, Apestigue, Victor, Martínez, Germán, Toledo, Daniel, Sullivan, Rob, Herkenhoff, Kenneth, de la Torre Juárez, Manuel, Richardson, Mark I., Stott, Alexander E., Murdoch, Naomi, Sánchez Lavega, Agustín María, 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, Mimoun, David, Tate, Christian, Bertrand, Tanguy, Bell, James, Maki, Justin N., Rodríguez Manfredi, José Antonio, Wiens, Roger C., Chide, Baptiste, Maurice, Sylvestre, Zorzano, María Paz, Mora Sotomayor, Luis, Baker, Mariah M., Banfield, Don, Plá García, Jorge, Beyssac, Olivier, Brown, Adrian, Clark, Ben, Lepinette, Alain, Montmessin, Franck, Fischer, Erik, Patel, Priyaben, Del Río Gaztelurrutia, María Teresa, Fouchet, Thierry, Francis, Raymond, Guzewich, Scott, Física aplicada I, Fisika aplikatua I, Newman, Claire E., Hueso Alonso, Ricardo, Lemmon, Mark T., Munguira Ruiz, Asier, Vicente Retortillo, Álvaro, Apestigue, Victor, Martínez, Germán, Toledo, Daniel, Sullivan, Rob, Herkenhoff, Kenneth, de la Torre Juárez, Manuel, Richardson, Mark I., Stott, Alexander E., Murdoch, Naomi, Sánchez Lavega, Agustín María, 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, Mimoun, David, Tate, Christian, Bertrand, Tanguy, Bell, James, Maki, Justin N., Rodríguez Manfredi, José Antonio, Wiens, Roger C., Chide, Baptiste, Maurice, Sylvestre, Zorzano, María Paz, Mora Sotomayor, Luis, Baker, Mariah M., Banfield, Don, Plá García, Jorge, Beyssac, Olivier, Brown, Adrian, Clark, Ben, Lepinette, Alain, Montmessin, Franck, Fischer, Erik, Patel, Priyaben, Del Río Gaztelurrutia, María Teresa, Fouchet, Thierry, Francis, Raymond, and Guzewich, Scott

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.

Published
2022

35. The Dark Side of Pluto

Author

Lauer, Tod R., primary, Spencer, John R., additional, Bertrand, Tanguy, additional, Beyer, Ross A., additional, Runyon, Kirby D,, additional, L White, Oliver, additional, Young, Leslie A., additional, Ennico, Kimberly, additional, McKinnon, William B., additional, Moore, Jeffrey M., additional, Olkin, Catherine B., additional, Stern, S. Alan, additional, and Weaver, Harold A., additional

Published
2021
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36. Triton: Topography and Geology of a Probable Ocean World with Comparison to Pluto and Charon

Author

Schenk, Paul, primary, Beddingfield, Chloe, additional, Bertrand, Tanguy, additional, Bierson, Carver, additional, Beyer, Ross, additional, Bray, Veronica, additional, Cruikshank, Dale, additional, Grundy, William, additional, Hansen, Candice, additional, Hofgartner, Jason, additional, Martin, Emily, additional, McKinnon, William, additional, Moore, Jeffrey, additional, Robbins, Stuart, additional, Runyon, Kirby, additional, Singer, Kelsi, additional, Spencer, John, additional, Stern, S., additional, and Stryk, Ted, additional

Published
2021
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37. Multi-model Meteorological and Aeolian Predictions for Mars 2020 and the Jezero Crater Region

Author

Física aplicada I, Fisika aplikatua I, Newman, C E, de la Torre Juárez, Manuel, Plá García, Jorge, Wilson, R. J., Lewis, S. R., Neary, L., Kahre, M. A., Forget, F., Spiga, A., Richardson, Mark I., Daerden, F., Bertrand, Tanguy, Viúdez Moreiras, Daniel, Sullivan, R., Sánchez Lavega, Agustín María, Chide, Baptiste, Rodríguez Manfredi, José Antonio, Física aplicada I, Fisika aplikatua I, Newman, C E, de la Torre Juárez, Manuel, Plá García, Jorge, Wilson, R. J., Lewis, S. R., Neary, L., Kahre, M. A., Forget, F., Spiga, A., Richardson, Mark I., Daerden, F., Bertrand, Tanguy, Viúdez Moreiras, Daniel, Sullivan, R., Sánchez Lavega, Agustín María, Chide, Baptiste, and Rodríguez Manfredi, José Antonio

Abstract

Nine simulations are used to predict the meteorology and aeolian activity of the Mars 2020 landing site region. Predicted seasonal variations of pressure and surface and atmospheric temperature generally agree. Minimum and maximum pressure is predicted at Ls similar to 145 degrees and 250 degrees, respectively. Maximum and minimum surface and atmospheric temperature are predicted at Ls similar to 180 degrees and 270 degrees, respectively; i.e., are warmest at northern fall equinox not summer solstice. Daily pressure cycles vary more between simulations, possibly due to differences in atmospheric dust distributions. Jezero crater sits inside and close to the NW rim of the huge Isidis basin, whose daytime upslope (similar to east-southeasterly) and nighttime downslope (similar to northwesterly) winds are predicted to dominate except around summer solstice, when the global circulation produces more southerly wind directions. Wind predictions vary hugely, with annual maximum speeds varying from 11 to 19 ms(-1) and daily mean wind speeds peaking in the first half of summer for most simulations but in the second half of the year for two. Most simulations predict net annual sand transport toward the WNW, which is generally consistent with aeolian observations, and peak sand fluxes in the first half of summer, with the weakest fluxes around winter solstice due to opposition between the global circulation and daytime upslope winds. However, one simulation predicts transport toward the NW, while another predicts fluxes peaking later and transport toward the WSW. Vortex activity is predicted to peak in summer and dip around winter solstice, and to be greater than at InSight and much greater than in Gale crater.

Published
2021

38. Exploration of the Ice Giant Systems: A White Paper for NASA's Planetary Science and Astrobiology Decadal Survey 2023-2032

Author

Beddingfield, Chloe, Li, Cheng, Atreya, Sushil, Beauchamp, Patricia, Cohen, Ian, Fortney, Jonathan, Hammel, Heidi, Hedman, Matthew, Hofstadter, Mark, Rymer, Abigail, Schenk, Paul, Showalter, Mark, Ahrens, Caitlin, Aplin, Karen, Arney, Giada, Aslam, Shahid, Azari, Abigail, Baillié, Kevin, Barth, Erika, BENNETT, christopher, Bertrand, Tanguy, Beyer, Ross, Bramson, Ali, Bierson, Carver, Brozovic, Marina, Brueshaber, Shawn, Bruce, Emma, Burr, Devon, Burratti, Bonnie, Byrne, Paul, Cao, Xin, Cartwright, Richard, Castillo-Rogez, Julie, Chancia, Rob, Chanover, Nancy, Clark, George, Coates, Andrew, Cochrane, Corey, Collins, Geoff, Colwell, Joshua, Crary, Frank, Cruikshank, Dale, Coustenis, Athena, Ćuk, Matija, Dahl, Emma, Daubar, Ingrid, DeColibus, David, DePater, Imke, Dhingra, Rajani, Dong, Chuanfei, Elder, Catherine, Emery, Joshua, Ermakov, Anton, Ferguson, Sierra, Fletcher, Leigh, French, Robert, Golder, Keenan, González, Felipe, Gordon, Mitchell, Grava, Cesare, Grodent, Denis, Grundy, Will, Hammond, Noah, Hawkins, Emily, Hayes, Alex, Helfenstein, Paul, Helled, Ravit, Hemingway, Douglas, Hendrix, Amanda, Higgins, Chuck, Hofmann, Amy, Holler, Bryan, Holt, Timothy, Hospodarsky, George, Howett, Carly, Hsu, Hsiang-Wen, Jackman, Caitriona, Jasinski, Jamie, Jha, Devanshu, Jia, Xianzhe, Jun, Insoo, Karkoschka, Erich, Kattenhorn, Simon, Kinczyk, Mallory, Kirchoff, Michelle, Kollmann, Peter, Kumar, Kartik, Keane, James, Kampf, Sascha, Leonard, Erin, Leung, Cecilia, Lissauer, Jack, Lopes, Rosaly, Lucas, Michael, Lucchetti, Alice, Mandt, Kathleen, Marouf, Essam, Martin, Emily, Masters, Adam, McGrath, Melissa, Michaels, Tim, Mitchell, Karl, Moran, Sarah, Moses, Julianne, Nenon, Quentin, Neveu, Marc, Nimmo, Francis, Nordheim, Tom, Pajola, Maurizio, Pappalardo, Robert, Paranicas, Chris, Patthoff, Alex, Paty, Carol, Person, Michael, Peterson, Georgia, Pinilla-Alonso, Noemi, Porter, Simon, Postberg, Frank, Probst, Alena, Quick, Lynnae, Regoli, Leonardo, Rivera-Valentín, Edgard, Roatsch, Thomas, Roberge, Aki, Roberts, James, Robbins, Stuart, Rodriguez, Sébastien, Roser, Joe, Roussos, Elias, Runyon, Kirby, Scipioni, Francesca, Scully, Jennifer, Singer, Kelsi, Soderlund, Krista, Sori, Mike, Spilker, Linda, Stern, Alan, Stryk, Ted, Styczinski, Marshall, Sulaiman, Ali, Tamayo, Daniel, Thieman, Jim, Tiscareno, Matthew, Tortora, Paolo, Turtle, Elizabeth, Umurhan, Orkan, Weiss, Benjamin, White, Oliver, Search for Extraterrestrial Intelligence Institute (SETI), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Physics::Space Physics, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics::Atmospheric and Oceanic Physics, Astrophysics - Earth and Planetary Astrophysics
Abstract

Ice giants are the only unexplored class of planet in our Solar System. Much that we currently know about these systems challenges our understanding of how planets, rings, satellites, and magnetospheres form and evolve. We assert that an ice giant Flagship mission with an atmospheric probe should be a priority for the decade 2023-2032.

Published
2020
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39. The methane cycles on Pluto over seasonal and astronomical timescales

Author

Bertrand, Tanguy, Forget, F., Umurhan, O.M., Moore, J.M., Young, L.A., Protopapa, S., Grundy, W.M., Schmitt, B., Dhingra, R.D., Binzel, R.P., Earle, A.M., Cruikshank, D.P., Stern, S.A., Weaver, H.A., Ennico, K., Olkin, C.B., Beyer, David, O'Brien, Paul, Withers, Gwen, Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris)-École normale supérieure - Paris (ENS Paris), NASA, Southwest Research Institute [Boulder] (SwRI), Lowell Observatory [Flagstaff], Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] (EAPS), Massachusetts Institute of Technology (MIT), NASA Ames Research Center (ARC), Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), and Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL)

Subjects
Brightness, glacier, 010504 meteorology & atmospheric sciences, Thermodynamic equilibrium, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, volatile transport, 01 natural sciences, Mantle (geology), Latitude, Astrobiology, paleoclimate, 0103 physical sciences, Paleoclimatology, Thermal, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), geography, geography.geographical_feature_category, Pluto, Modeling, Astronomy and Astrophysics, Glacier, CH4 ice, GCM, 13. Climate action, Space and Planetary Science, atmosphere, Geology, Astrophysics - Earth and Planetary Astrophysics
Abstract

New Horizons observations suggest that CH4 on Pluto has a complex history, involving reservoirs of different composition, thickness and stability controlled by volatile processes occurring on different timescales. In order to interpret these observations, we use a Pluto volatile transport model able to simulate the cycles of N2 and CH4 ices over millions of years. By assuming fixed solid mixing ratios, we explore how changes in surface albedos, emissivities and thermal inertias impact volatile transport. This work is therefore a direct and natural continuation of the work by Bertrand et al. (2018), which only explored the N2 cycles. Results show that bright CH4 deposits can create cold traps for N2 ice outside Sputnik Planitia, leading to a strong coupling between the N2 and CH4 cycles. Depending on the assumed albedo for CH4 ice, the model predicts CH4 ice accumulation (1) at the same equatorial latitudes where the Bladed Terrain Deposits are observed, supporting the idea that these CH4-rich deposits are massive and perennial, or (2) at mid-latitudes (25{\deg}N-70{\deg}N), forming a thick mantle which is consistent with New Horizons observations. In our simulations, both CH4 ice reservoirs are not in an equilibrium state and either one can dominate the other over long timescales, depending on the assumptions made for the CH4 albedo. This suggests that long-term volatile transport exists between the observed reservoirs. The model also reproduces the formation of N2 deposits at mid-latitudes and in the equatorial depressions surrounding the Bladed Terrain, as observed by New Horizons. At the poles, only seasonal CH4 and N2 deposits are obtained in Pluto's current orbital configuration. Finally, we show that Pluto's atmosphere always contained, over the last astronomical cycles, enough gaseous CH4 to absorb most of the incoming Lyman-flux., Comment: Accepted in Icarus

Published
2019
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40. Dunes on Pluto

Author

Telfer, Matt W., Parteli, Eric J. R., Radebaugh, Jani, Beyer, Ross A., Bertrand, Tanguy, Forget, Francois, Nimmo, Francis, Grundy, Will M., Moore, Jeffrey M., Stern, S. Alan, Spencer, John, Lauer, Tod R., Earle, Alissa M., Binzel, Richard P., Weaver, Hal A., Olkin, Cathy B., Young, Leslie A., Ennico, Kimberly, Runyon, Kirby, Telfer, Matt W., Parteli, Eric J. R., Radebaugh, Jani, Beyer, Ross A., Bertrand, Tanguy, Forget, Francois, Nimmo, Francis, Grundy, Will M., Moore, Jeffrey M., Stern, S. Alan, Spencer, John, Lauer, Tod R., Earle, Alissa M., Binzel, Richard P., Weaver, Hal A., Olkin, Cathy B., Young, Leslie A., Ennico, Kimberly, and Runyon, Kirby

Abstract

The surface of Pluto is more geologically diverse and dynamic than had been expected, but the role of its tenuous atmosphere in shaping the landscape remains unclear. We describe observations from the New Horizons spacecraft of regularly spaced, linear ridges whose morphology, distribution, and orientation are consistent with being transverse dunes. These are located close to mountainous regions and are orthogonal to nearby wind streaks. We demonstrate that the wavelength of the dunes (-0.4 to 1 kilometer) is best explained by the deposition of sand-sized (-200 to -300 micrometer) particles of methane ice in moderate winds (<10 meters per second). The undisturbed morphology of the dunes, and relationships with the underlying convective glacial ice, imply that the dunes have formed in the very recent geological past.

Published
2018

41. An intercomparison of Large-Eddy Simulations of the Martian daytime convective boundary layer.

Author

Bertrand, Tanguy, Spiga, Aymeric, Rafkin, Scot, Colaitis, Arnaud, Forget, François, and Millour, Ehouarn

Subjects
*ATMOSPHERIC boundary layer, *LARGE eddy simulation models, *ATMOSPHERIC turbulence, *MARS (Planet), *ROBOTICS, *PREDICTION models
Abstract

Large-Eddy Simulations (LES) for Mars resolve the Planetary Boundary Layer (PBL) turbulent dynamics by using a very fine horizontal resolution of a few tens of meters. LES modeling is becoming a more and more useful tool to prepare the robotic exploration of Mars by providing means to evaluate the intensity of convective plumes and vortices, horizontal wind gustiness, and turbulent fluctuations of temperature in the Martian PBL. In such context, and given the relative paucity of turbulence-related measurements on Mars, an intercomparison of LES models is a fruitful way to evaluate the models' predictions and to indicate possible areas of improvement. Thus, to prepare the landing of the ExoMars Schiaparelli lander (also named ExoMars Demonstrator Module, EDM), scheduled for October 2016, the results of the Laboratoire de Météorologie Dynamique (LMD) and South-West Research Institute (SwRI) LES models have been compared. The objective of this study is to determine the range of uncertainties, and dispersions, of the two numerical models' predictions, for the critical phase of the spacecraft's descent in the Martian daytime turbulent PBL. First, a strategy is defined to ensure similar radiative forcing in both the LMD and SwRI models. Then, LES are performed over a flat terrain with and without large-scale ambient horizontal wind. The LMD and SwRI Martian LES models predict similar temporal evolution of the PBL and organization in the horizontal and vertical wind fields. However, the convective motions in the daytime PBL are more vigorous by a factor 1.5-2 in SwRI results than in LMD results, independently of the presence or not of ambient horizontal wind. This discrepancy is further investigated through sensitivity studies to surface conditions, ambient wind, and airborne dust loading. [ABSTRACT FROM AUTHOR]

Published
2016
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42. Toward More Realistic Simulation and Prediction of Dust Storms on Mars

Author

Newman, Claire, Bertrand, Tanguy, Battalio, Joseph, Day, Mackenzie, Juárez, Manuel De La Torre, Elrod, Meredith K., Esposito, Francesca, Fenton, Lori, Gebhardt, Claus, Greybush, Steven J., Guzewich, Scott D., Kahanpää, Henrik, Kahre, Melinda, Karatekin, Özgür, Jackson, Brian, Lapotre, Mathieu, Lee, Christopher, Lewis, Stephen R., Lorenz, Ralph D., Martínez, Germán, Martin-Torres, Javier, Mischna, Michael A., Montabone, Luca, Neakrase, Lynn, Pankine, Alexey, Pla-Garcia, Jorge, Read, Peter L., Smith, Isaac B., Smith, Michael D., Soto, Alejandro, Spiga, Aymeric, Swann, Christy, Tamppari, Leslie, Temel, Orkun, Moreiras, Daniel Viudez, Wellington, Danika, Wolkenberg, Paulina, Wurm, Gerhard, Zorzano, María-Paz, Newman, Claire, Bertrand, Tanguy, Battalio, Joseph, Day, Mackenzie, Juárez, Manuel De La Torre, Elrod, Meredith K., Esposito, Francesca, Fenton, Lori, Gebhardt, Claus, Greybush, Steven J., Guzewich, Scott D., Kahanpää, Henrik, Kahre, Melinda, Karatekin, Özgür, Jackson, Brian, Lapotre, Mathieu, Lee, Christopher, Lewis, Stephen R., Lorenz, Ralph D., Martínez, Germán, Martin-Torres, Javier, Mischna, Michael A., Montabone, Luca, Neakrase, Lynn, Pankine, Alexey, Pla-Garcia, Jorge, Read, Peter L., Smith, Isaac B., Smith, Michael D., Soto, Alejandro, Spiga, Aymeric, Swann, Christy, Tamppari, Leslie, Temel, Orkun, Moreiras, Daniel Viudez, Wellington, Danika, Wolkenberg, Paulina, Wurm, Gerhard, and Zorzano, María-Paz

Abstract

Global dust storms have major implications for the past and present climate, geologic history, habitability, and future exploration of Mars. Yet their mysterious origins mean we remain unable to realistically simulate or predict them. We identify four key Knowledge Gaps and make four Recommendations to make progress in the next decade.

43. Toward More Realistic Simulation and Prediction of Dust Storms on Mars

Author

Newman, Claire, Bertrand, Tanguy, Battalio, Joseph, Day, Mackenzie, Juárez, Manuel De La Torre, Elrod, Meredith K., Esposito, Francesca, Fenton, Lori, Gebhardt, Claus, Greybush, Steven J., Guzewich, Scott D., Kahanpää, Henrik, Kahre, Melinda, Karatekin, Özgür, Jackson, Brian, Lapotre, Mathieu, Lee, Christopher, Lewis, Stephen R., Lorenz, Ralph D., Martínez, Germán, Martin-Torres, Javier, Mischna, Michael A., Montabone, Luca, Neakrase, Lynn, Pankine, Alexey, Pla-Garcia, Jorge, Read, Peter L., Smith, Isaac B., Smith, Michael D., Soto, Alejandro, Spiga, Aymeric, Swann, Christy, Tamppari, Leslie, Temel, Orkun, Moreiras, Daniel Viudez, Wellington, Danika, Wolkenberg, Paulina, Wurm, Gerhard, Zorzano, María-Paz, Newman, Claire, Bertrand, Tanguy, Battalio, Joseph, Day, Mackenzie, Juárez, Manuel De La Torre, Elrod, Meredith K., Esposito, Francesca, Fenton, Lori, Gebhardt, Claus, Greybush, Steven J., Guzewich, Scott D., Kahanpää, Henrik, Kahre, Melinda, Karatekin, Özgür, Jackson, Brian, Lapotre, Mathieu, Lee, Christopher, Lewis, Stephen R., Lorenz, Ralph D., Martínez, Germán, Martin-Torres, Javier, Mischna, Michael A., Montabone, Luca, Neakrase, Lynn, Pankine, Alexey, Pla-Garcia, Jorge, Read, Peter L., Smith, Isaac B., Smith, Michael D., Soto, Alejandro, Spiga, Aymeric, Swann, Christy, Tamppari, Leslie, Temel, Orkun, Moreiras, Daniel Viudez, Wellington, Danika, Wolkenberg, Paulina, Wurm, Gerhard, and Zorzano, María-Paz

Abstract

Global dust storms have major implications for the past and present climate, geologic history, habitability, and future exploration of Mars. Yet their mysterious origins mean we remain unable to realistically simulate or predict them. We identify four key Knowledge Gaps and make four Recommendations to make progress in the next decade.

44. Compositionally and density stratified igneous terrain in Jezero crater, Mars.

Author

Wiens RC, Udry A, Beyssac O, Quantin-Nataf C, Mangold N, Cousin A, Mandon L, Bosak T, Forni O, McLennan SM, Sautter V, Brown A, Benzerara K, Johnson JR, Mayhew L, Maurice S, Anderson RB, Clegg SM, Crumpler L, Gabriel TSJ, Gasda P, Hall J, Horgan BHN, Kah L, Legett C 4th, Madariaga JM, Meslin PY, Ollila AM, Poulet F, Royer C, Sharma SK, Siljeström S, Simon JI, Acosta-Maeda TE, Alvarez-Llamas C, Angel SM, Arana G, Beck P, Bernard S, Bertrand T, Bousquet B, Castro K, Chide B, Clavé E, Cloutis E, Connell S, Dehouck E, Dromart G, Fischer W, Fouchet T, Francis R, Frydenvang J, Gasnault O, Gibbons E, Gupta S, Hausrath EM, Jacob X, Kalucha H, Kelly E, Knutsen E, Lanza N, Laserna J, Lasue J, Le Mouélic S, Leveille R, Lopez Reyes G, Lorenz R, Manrique JA, Martinez-Frias J, McConnochie T, Melikechi N, Mimoun D, Montmessin F, Moros J, Murdoch N, Pilleri P, Pilorget C, Pinet P, Rapin W, Rull F, Schröder S, Shuster DL, Smith RJ, Stott AE, Tarnas J, Turenne N, Veneranda M, Vogt DS, Weiss BP, Willis P, Stack KM, Williford KH, and Farley KA

Abstract

Before Perseverance, Jezero crater's floor was variably hypothesized to have a lacustrine, lava, volcanic airfall, or aeolian origin. SuperCam observations in the first 286 Mars days on Mars revealed a volcanic and intrusive terrain with compositional and density stratification. The dominant lithology along the traverse is basaltic, with plagioclase enrichment in stratigraphically higher locations. Stratigraphically lower, layered rocks are richer in normative pyroxene. The lowest observed unit has the highest inferred density and is olivine-rich with coarse (1.5 millimeters) euhedral, relatively unweathered grains, suggesting a cumulate origin. This is the first martian cumulate and shows similarities to martian meteorites, which also express olivine disequilibrium. Alteration materials including carbonates, sulfates, perchlorates, hydrated silicates, and iron oxides are pervasive but low in abundance, suggesting relatively brief lacustrine conditions. Orbital observations link the Jezero floor lithology to the broader Nili-Syrtis region, suggesting that density-driven compositional stratification is a regional characteristic.

Published
2022
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