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Ross B, Haussener S, Brinkert K. Assessment of the technological viability of photoelectrochemical devices for oxygen and fuel production on Moon and Mars. Nat Commun 2023; 14:3141. [PMID: 37280222 DOI: 10.1038/s41467-023-38676-2] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 10/25/2022] [Accepted: 05/09/2023] [Indexed: 06/08/2023] Open
Abstract
Human deep space exploration is presented with multiple challenges, such as the reliable, efficient and sustainable operation of life support systems. The production and recycling of oxygen, carbon dioxide (CO2) and fuels are hereby key, as a resource resupply will not be possible. Photoelectrochemical (PEC) devices are investigated for the light-assisted production of hydrogen and carbon-based fuels from CO2 within the green energy transition on Earth. Their monolithic design and the sole reliance on solar energy makes them attractive for applications in space. Here, we establish the framework to evaluate PEC device performances on Moon and Mars. We present a refined Martian solar irradiance spectrum and establish the thermodynamic and realistic efficiency limits of solar-driven lunar water-splitting and Martian carbon dioxide reduction (CO2R) devices. Finally, we discuss the technological viability of PEC devices in space by assessing the performance combined with solar concentrator devices and explore their fabrication via in-situ resource utilization.
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Affiliation(s)
- Byron Ross
- Department of Chemistry, University of Warwick, Coventry, CV4 7AL, UK
| | - Sophia Haussener
- Institute of Mechanical Engineering, Ecole Polytechnique Fédérale de Lausanne (EPFL), 1015, Lausanne, Switzerland
| | - Katharina Brinkert
- Department of Chemistry, University of Warwick, Coventry, CV4 7AL, UK.
- ZARM - Center for Applied Space Technology and Microgravity, University of Bremen, 28359, Bremen, Germany.
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2
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Bell JF, Maki JN, Alwmark S, Ehlmann BL, Fagents SA, Grotzinger JP, Gupta S, Hayes A, Herkenhoff KE, Horgan BHN, Johnson JR, Kinch KB, Lemmon MT, Madsen MB, Núñez JI, Paar G, Rice M, Rice JW, Schmitz N, Sullivan R, Vaughan A, Wolff MJ, Bechtold A, Bosak T, Duflot LE, Fairén AG, Garczynski B, Jaumann R, Merusi M, Million C, Ravanis E, Shuster DL, Simon J, St. Clair M, Tate C, Walter S, Weiss B, Bailey AM, Bertrand T, Beyssac O, Brown AJ, Caballo-Perucha P, Caplinger MA, Caudill CM, Cary F, Cisneros E, Cloutis EA, Cluff N, Corlies P, Crawford K, Curtis S, Deen R, Dixon D, Donaldson C, Barrington M, Ficht M, Fleron S, Hansen M, Harker D, Howson R, Huggett J, Jacob S, Jensen E, Jensen OB, Jodhpurkar M, Joseph J, Juarez C, Kah LC, Kanine O, Kristensen J, Kubacki T, Lapo K, Magee A, Maimone M, Mehall GL, Mehall L, Mollerup J, Viúdez-Moreiras D, Paris K, Powell KE, Preusker F, Proton J, Rojas C, Sallurday D, Saxton K, Scheller E, Seeger CH, Starr M, Stein N, Turenne N, Van Beek J, Winhold AG, Yingling R. Geological, multispectral, and meteorological imaging results from the Mars 2020 Perseverance rover in Jezero crater. SCIENCE ADVANCES 2022; 8:eabo4856. [PMID: 36417517 PMCID: PMC9683734 DOI: 10.1126/sciadv.abo4856] [Citation(s) in RCA: 4] [Impact Index Per Article: 2.0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 02/15/2022] [Accepted: 10/20/2022] [Indexed: 06/15/2023]
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 fine-grained 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.
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Affiliation(s)
- James F. Bell
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85281, USA
| | - Justin N. Maki
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - Sanna Alwmark
- Niels Bohr Institute, University of Copenhagen, 2100 Copenhagen, Denmark
- Department of Geology, Lund University, 22362 Lund, Sweden
| | - Bethany L. Ehlmann
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - Sarah A. Fagents
- Hawai’i Institute of Geophysics and Planetology, University of Hawaii, Honolulu, HI 96822, USA
| | | | - Sanjeev Gupta
- Department of Earth Science and Engineering, Imperial College London, London, UK
| | - Alexander Hayes
- Department of Astronomy, Cornell University, Ithaca, NY 14850, USA
| | | | - Briony H. N. Horgan
- Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN 47907, USA
| | - Jeffrey R. Johnson
- Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA
| | - Kjartan B. Kinch
- Niels Bohr Institute, University of Copenhagen, 2100 Copenhagen, Denmark
| | | | - Morten B. Madsen
- Niels Bohr Institute, University of Copenhagen, 2100 Copenhagen, Denmark
| | - Jorge I. Núñez
- Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA
| | | | - Melissa Rice
- Western Washington University, Bellingham, WA 98225, USA
| | - James W. Rice
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85281, USA
| | | | - Robert Sullivan
- Department of Astronomy, Cornell University, Ithaca, NY 14850, USA
| | - Alicia Vaughan
- USGS Astrogeology Science Center, Flagstaff, AZ 86001, USA
| | | | - Andreas Bechtold
- Department of Lithospheric Research, University of Vienna, 1090 Vienna, Austria
- Austrian Academy of Sciences, Vienna 1010, Austria
| | - Tanja Bosak
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
| | | | - Alberto G. Fairén
- Department of Astronomy, Cornell University, Ithaca, NY 14850, USA
- Astrobiology Center (CSIC-INTA), Madrid, Spain
| | - Brad Garczynski
- Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN 47907, USA
| | - Ralf Jaumann
- Institute for Geological Sciences, Freie Universitaet Berlin, 14195 Berlin, Germany
| | - Marco Merusi
- Niels Bohr Institute, University of Copenhagen, 2100 Copenhagen, Denmark
| | | | - Eleni Ravanis
- Hawai’i Institute of Geophysics and Planetology, University of Hawaii, Honolulu, HI 96822, USA
| | - David L. Shuster
- Department of Earth and Planetary Science, University of California, Berkeley, Berkeley, CA 94720, USA
| | - Justin Simon
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | | | - Christian Tate
- Department of Astronomy, Cornell University, Ithaca, NY 14850, USA
| | - Sebastian Walter
- Institute for Geological Sciences, Freie Universitaet Berlin, 14195 Berlin, Germany
| | - Benjamin Weiss
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
| | - Alyssa M. Bailey
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85281, USA
| | | | - Olivier Beyssac
- Institut de Minéralogie, Physique des Matériaux et Cosmochimie, CNRS, Muséum National d’Histoire Naturelle, Sorbonne University, Paris 75005, France
| | | | | | | | | | - Francesca Cary
- Hawai’i Institute of Geophysics and Planetology, University of Hawaii, Honolulu, HI 96822, USA
| | - Ernest Cisneros
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85281, USA
| | | | - Nathan Cluff
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85281, USA
| | - Paul Corlies
- Department of Astronomy, Cornell University, Ithaca, NY 14850, USA
| | - Kelsie Crawford
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85281, USA
| | - Sabrina Curtis
- Western Washington University, Bellingham, WA 98225, USA
| | - Robert Deen
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - Darian Dixon
- Malin Space Science Systems Inc., San Diego, CA 92121, USA
| | | | - Megan Barrington
- Department of Astronomy, Cornell University, Ithaca, NY 14850, USA
| | - Michelle Ficht
- Malin Space Science Systems Inc., San Diego, CA 92121, USA
| | | | | | - David Harker
- Malin Space Science Systems Inc., San Diego, CA 92121, USA
| | - Rachel Howson
- Malin Space Science Systems Inc., San Diego, CA 92121, USA
| | - Joshua Huggett
- Malin Space Science Systems Inc., San Diego, CA 92121, USA
| | - Samantha Jacob
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85281, USA
| | - Elsa Jensen
- Malin Space Science Systems Inc., San Diego, CA 92121, USA
| | - Ole B. Jensen
- Niels Bohr Institute, University of Copenhagen, 2100 Copenhagen, Denmark
| | - Mohini Jodhpurkar
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85281, USA
| | - Jonathan Joseph
- Department of Astronomy, Cornell University, Ithaca, NY 14850, USA
| | | | - Linda C. Kah
- Department of Earth and Planetary Sciences, University of Tennessee, Knoxville, TN 37916, USA
| | - Oak Kanine
- California Institute of Technology, Pasadena, CA 91125, USA
| | | | - Tex Kubacki
- Malin Space Science Systems Inc., San Diego, CA 92121, USA
| | - Kristiana Lapo
- Western Washington University, Bellingham, WA 98225, USA
| | - Angela Magee
- Malin Space Science Systems Inc., San Diego, CA 92121, USA
| | | | - Greg L. Mehall
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85281, USA
| | - Laura Mehall
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85281, USA
| | - Jess Mollerup
- Western Washington University, Bellingham, WA 98225, USA
| | - Daniel Viúdez-Moreiras
- Astrobiology Center (CSIC-INTA), Madrid, Spain
- National Institute for Aerospace Technology, Madrid, Spain
| | - Kristen Paris
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85281, USA
| | - Kathryn E. Powell
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85281, USA
| | | | | | - Corrine Rojas
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85281, USA
| | | | - Kim Saxton
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - Eva Scheller
- California Institute of Technology, Pasadena, CA 91125, USA
| | | | - Mason Starr
- Malin Space Science Systems Inc., San Diego, CA 92121, USA
| | - Nathan Stein
- California Institute of Technology, Pasadena, CA 91125, USA
| | | | - Jason Van Beek
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - Andrew G. Winhold
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85281, USA
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3
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Oliva F, D’Aversa E, Bellucci G, Carrozzo FG, Ruiz Lozano L, Altieri F, Thomas IR, Karatekin O, Cruz Mermy G, Schmidt F, Robert S, Vandaele AC, Daerden F, Ristic B, Patel MR, López‐Moreno J, Sindoni G. Martian CO 2 Ice Observation at High Spectral Resolution With ExoMars/TGO NOMAD. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2022; 127:e2021JE007083. [PMID: 35865508 PMCID: PMC9286783 DOI: 10.1029/2021je007083] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 10/04/2021] [Revised: 04/16/2022] [Accepted: 04/19/2022] [Indexed: 06/15/2023]
Abstract
The Nadir and Occultation for MArs Discovery (NOMAD) instrument suite aboard ExoMars/Trace Gas Orbiter spacecraft is mainly conceived for the study of minor atmospheric species, but it also offers the opportunity to investigate surface composition and aerosols properties. We investigate the information content of the Limb, Nadir, and Occultation (LNO) infrared channel of NOMAD and demonstrate how spectral orders 169, 189, and 190 can be exploited to detect surface CO2 ice. We study the strong CO2 ice absorption band at 2.7 μm and the shallower band at 2.35 μm taking advantage of observations across Martian Years 34 and 35 (March 2018 to February 2020), straddling a global dust storm. We obtain latitudinal-seasonal maps for CO2 ice in both polar regions, in overall agreement with predictions by a general climate model and with the Mars Express/OMEGA spectrometer Martian Years 27 and 28 observations. We find that the narrow 2.35 μm absorption band, spectrally well covered by LNO order 189, offers the most promising potential for the retrieval of CO2 ice microphysical properties. Occurrences of CO2 ice spectra are also detected at low latitudes and we discuss about their interpretation as daytime high altitude CO2 ice clouds as opposed to surface frost. We find that the clouds hypothesis is preferable on the basis of surface temperature, local time and grain size considerations, resulting in the first detection of CO2 ice clouds through the study of this spectral range. Through radiative transfer considerations on these detections we find that the 2.35 μm absorption feature of CO2 ice clouds is possibly sensitive to nm-sized ice grains.
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Affiliation(s)
- F. Oliva
- Istituto di Astrofisica e Planetologia Spaziali (IAPS/INAF)RomeItaly
| | - E. D’Aversa
- Istituto di Astrofisica e Planetologia Spaziali (IAPS/INAF)RomeItaly
| | - G. Bellucci
- Istituto di Astrofisica e Planetologia Spaziali (IAPS/INAF)RomeItaly
| | - F. G. Carrozzo
- Istituto di Astrofisica e Planetologia Spaziali (IAPS/INAF)RomeItaly
| | - L. Ruiz Lozano
- Université Catholique de Louvain‐la‐Neuve (UCLouvain)Louvain‐la‐NeuveBelgium
- Royal Observatory of BelgiumBrusselsBelgium
| | - F. Altieri
- Istituto di Astrofisica e Planetologia Spaziali (IAPS/INAF)RomeItaly
| | - I. R. Thomas
- Royal Belgian Institute for Space Aeronomy (IASB‐BIRA)BrusselsBelgium
| | | | | | - F. Schmidt
- CNRSGEOPSUniversité Paris‐SaclayOrsayFrance
- Institut Universitaire de France (IUF)ParisFrance
| | - S. Robert
- Université Catholique de Louvain‐la‐Neuve (UCLouvain)Louvain‐la‐NeuveBelgium
- Royal Belgian Institute for Space Aeronomy (IASB‐BIRA)BrusselsBelgium
| | - A. C. Vandaele
- Royal Belgian Institute for Space Aeronomy (IASB‐BIRA)BrusselsBelgium
| | - F. Daerden
- Royal Belgian Institute for Space Aeronomy (IASB‐BIRA)BrusselsBelgium
| | - B. Ristic
- Royal Belgian Institute for Space Aeronomy (IASB‐BIRA)BrusselsBelgium
| | - M. R. Patel
- School of Physical SciencesThe Open UniversityMilton KeynesUK
| | - J.‐J. López‐Moreno
- Instituto de Astrofìsica de Andalucia (IAA)Consejo Superior de Investigaciones Científicas (CSIC)GranadaSpain
| | - G. Sindoni
- Agenzia Spaziale Italiana (ASI)RomeItaly
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4
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Streeter PM, Sellers G, Wolff MJ, Mason JP, Patel MR, Lewis SR, Holmes JA, Daerden F, Thomas IR, Ristic B, Willame Y, Depiesse C, Vandaele AC, Bellucci G, López‐Moreno JJ. Vertical Aerosol Distribution and Mesospheric Clouds From ExoMars UVIS. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2022; 127:e2021JE007065. [PMID: 35865506 PMCID: PMC9286791 DOI: 10.1029/2021je007065] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 09/27/2021] [Revised: 03/03/2022] [Accepted: 04/07/2022] [Indexed: 06/15/2023]
Abstract
The vertical opacity structure of the martian atmosphere is important for understanding the distribution of ice (water and carbon dioxide) and dust. We present a new data set of extinction opacity profiles from the NOMAD/UVIS spectrometer aboard the ExoMars Trace Gas Orbiter, covering one and a half Mars Years (MY) including the MY 34 Global Dust Storm and several regional dust storms. We discuss specific mesospheric cloud features and compare with existing literature and a Mars Global Climate Model (MGCM) run with data assimilation. Mesospheric opacity features, interpreted to be water ice, were present during the global and regional dust events and correlate with an elevated hygropause in the MGCM, providing evidence that regional dust storms can boost transport of vapor to mesospheric altitudes (with potential implications for atmospheric escape). The season of the dust storms also had an apparent impact on the resulting lifetime of the cloud features, with events earlier in the dusty season correlating with longer-lasting mesospheric cloud layers. Mesospheric opacity features were also present during the dusty season even in the absence of regional dust storms, and interpreted to be water ice based on previous literature. The assimilated MGCM temperature structure agreed well with the UVIS opacities, but the MGCM opacity field struggled to reproduce mesospheric ice features, suggesting a need for further development of water ice parameterizations. The UVIS opacity data set offers opportunities for further research into the vertical aerosol structure of the martian atmosphere, and for validation of how this is represented in numerical models.
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Affiliation(s)
| | - Graham Sellers
- School of Physical SciencesThe Open UniversityMilton KeynesUK
| | | | | | - Manish R. Patel
- School of Physical SciencesThe Open UniversityMilton KeynesUK
- Space Science and Technology DepartmentScience and Technology Facilities CouncilRutherford Appleton LaboratoryOxfordshireUK
| | | | - James A. Holmes
- School of Physical SciencesThe Open UniversityMilton KeynesUK
| | - Frank Daerden
- Royal Belgian Institute for Space Aeronomy (IASB‐BIRA)BrusselsBelgium
| | - Ian R. Thomas
- Royal Belgian Institute for Space Aeronomy (IASB‐BIRA)BrusselsBelgium
| | - Bojan Ristic
- Royal Belgian Institute for Space Aeronomy (IASB‐BIRA)BrusselsBelgium
| | - Yannick Willame
- Royal Belgian Institute for Space Aeronomy (IASB‐BIRA)BrusselsBelgium
| | - Cédric Depiesse
- Royal Belgian Institute for Space Aeronomy (IASB‐BIRA)BrusselsBelgium
| | | | | | - José Juan López‐Moreno
- Instituto de Astrofìsica de Andalucía (IAA)Consejo Superior de Investigaciones Científicas (CSIC)GranadaSpain
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5
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Zastrow AM, Glotch TD. Distinct Carbonate Lithologies in Jezero Crater, Mars. GEOPHYSICAL RESEARCH LETTERS 2021; 48:e2020GL092365. [PMID: 34219844 PMCID: PMC8243932 DOI: 10.1029/2020gl092365] [Citation(s) in RCA: 4] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 12/31/2020] [Revised: 04/03/2021] [Accepted: 04/08/2021] [Indexed: 05/20/2023]
Abstract
Jezero crater is the landing site for the Mars 2020 Perseverance rover. The Noachian-aged crater has undergone several periods of fluvial and lacustrine activity and phyllosilicate- and carbonate-bearing rocks were formed and emplaced as a result. It also contains a portion of the regional Nili Fossae olivine-carbonate unit. In this work, we performed spectral mixture analysis of visible/near-infrared hyperspectral imagery over Jezero. We modeled carbonate abundances up to ∼35% and identified three distinct units containing different carbonate phases. Our work also shows that the olivine in Jezero is predominantly restricted to aeolian deposits overlying the carbonate rocks. The diversity of carbonate phases in Jezero points to multiple periods of carbonate formation under varying conditions.
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Mandon L, Parkes Bowen A, Quantin-Nataf C, Bridges JC, Carter J, Pan L, Beck P, Dehouck E, Volat M, Thomas N, Cremonese G, Tornabene LL, Thollot P. Morphological and Spectral Diversity of the Clay-Bearing Unit at the ExoMars Landing Site Oxia Planum. ASTROBIOLOGY 2021; 21:464-480. [PMID: 33646016 DOI: 10.1089/ast.2020.2292] [Citation(s) in RCA: 3] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/12/2023]
Abstract
The European Space Agency and Roscosmos' ExoMars rover mission, which is planned to land in the Oxia Planum region, will be dedicated to exobiology studies at the surface and subsurface of Mars. Oxia Planum is a clay-bearing site that has preserved evidence of long-term interaction with water during the Noachian era. Fe/Mg-rich phyllosilicates have previously been shown to occur extensively throughout the landing area. Here, we analyze data from the High Resolution Imaging Science Experiment (HiRISE) and from the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) instruments onboard NASA's Mars Reconnaissance Orbiter and the Colour and Stereo Surface Imaging System (CaSSIS) onboard ESA's Trace Gas Orbiter to characterize, at a high spatial resolution, the morphological and spectral variability of Oxia Planum's surface deposits. Two main types of bedrocks are identified within the clay-bearing, fractured unit observed throughout the landing site: (1) an orange type in HiRISE correlated with the strongest detections of secondary minerals (dominated by Fe/Mg-rich clay minerals) with, in some locations, an additional spectral absorption near 2.5 μm, suggesting the mixture with an additional mineral, plausibly carbonate or another type of clay mineral; (2) a more bluish bedrock associated with weaker detections of secondary minerals, which exhibits at certain locations a ∼1 μm broad absorption feature consistent with olivine. Coanalysis of the same terrains with the recently acquired CaSSIS images confirms the variability in the color and spectral properties of the fractured unit. Of interest for the ExoMars mission, both types of bedrocks are extensively outcropping in the Oxia Planum region, and the one corresponding to the most intense spectral signals of clay minerals (the primary scientific target) is well exposed within the landing area, including near its center.
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Affiliation(s)
- Lucia Mandon
- Univ Lyon, Univ Lyon 1, ENSL, CNRS, LGL-TPE, F-69622, Villeurbanne, France
| | - Adam Parkes Bowen
- Space Research Centre, University of Leicester, Leicester, United Kingdom
| | | | - John C Bridges
- Space Research Centre, University of Leicester, Leicester, United Kingdom
| | - John Carter
- Institut d'Astrophysique Spatiale, CNRS, Université Paris-Sud, Orsay, France
| | - Lu Pan
- Univ Lyon, Univ Lyon 1, ENSL, CNRS, LGL-TPE, F-69622, Villeurbanne, France
| | - Pierre Beck
- Université Grenoble Alpes, CNRS, IPAG, UMR 5274, F-38041, Grenoble, France
- Institut Universitaire de France, Paris, France
| | - Erwin Dehouck
- Univ Lyon, Univ Lyon 1, ENSL, CNRS, LGL-TPE, F-69622, Villeurbanne, France
| | - Matthieu Volat
- Univ Lyon, Univ Lyon 1, ENSL, CNRS, LGL-TPE, F-69622, Villeurbanne, France
| | - Nicolas Thomas
- Physikalisches Institut, Sidlerstr. 5, University of Bern, 3012 Bern, Switzerland
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DEM Based Study on Shielded Astronomical Solar Radiation and Possible Sunshine Duration under Terrain Influences on Mars by Using Spectral Methods. ISPRS INTERNATIONAL JOURNAL OF GEO-INFORMATION 2021. [DOI: 10.3390/ijgi10020056] [Citation(s) in RCA: 3] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 01/10/2023]
Abstract
Solar radiation may be shielded by the terrain relief before reaching the Martian surface, especially over some rugged terrains. Yet, to date, no comprehensive studies on the spatial structure of shielded astronomical solar radiation (SASR) and the possible sunshine duration (PSD) on Mars have been conducted by previous researchers. Previous studies generally ignored the influences of the terrain on the SASR and PSD, which resulted in a corresponding unexplored field on SASR. The purpose of this paper is to study the Martian spatial-temporal structure of SASR and the PSD under terrain influences. In this paper, the theory of Earth’s SASR, the previous Martian SASR model and the theory of planetary science were combined to propose the SASR model that can be applied to Mars. Then, with the spectrum method theory of geography, we defined two new concepts of spectrums to explore the spatial-temporal distribution of SASR and PSD in different Martian landforms. We found SASR and PSD on Mars were significantly influenced by terrain relief and latitude and showed sufficient regularity, which can be concluded as a gradual attenuation with terrain relief and a regularity of latitude anisotropy. The latitude anisotropy feature is a manifestation of the terrain shielding effect. With the latitude varying, SASR and PSD at different temporal scale generally showed different features with those of Earth, which may be attributed to the imbalanced seasons caused by Martian moving orbits and velocity. Compared to PSD, SASR showed more regular variation under terrain relief and was more influenced by the terrain relief which revealed that SASR is more sensitive to terrain relief than PSD. Additionally, the critical area is a quantitative index to reflect the stable spatial structure of SASR and PSD in different landforms and may be viewed as the minimum test region of sample areas. The corresponding result of the experiments herein indicated that either spectrum can effectively depict the spatial-temporal distribution of SASR and PSD on Mars under terrain relief and deepen the understanding of the variation of SASR and PSD influences by terrain. The critical area of either spectrum can be employed to explore and determine the stable spatial structure of SASR and PSD in different landforms. The proposed Martian SASR model and the new spectral method theory shed new light on revealing the spatial-temporal structure of SASR and PSD under terrain influences on Mars.
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8
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Bell JF, Maki JN, Mehall GL, Ravine MA, Caplinger MA, Bailey ZJ, Brylow S, Schaffner JA, Kinch KM, Madsen MB, Winhold A, Hayes AG, Corlies P, Tate C, Barrington M, Cisneros E, Jensen E, Paris K, Crawford K, Rojas C, Mehall L, Joseph J, Proton JB, Cluff N, Deen RG, Betts B, Cloutis E, Coates AJ, Colaprete A, Edgett KS, Ehlmann BL, Fagents S, Grotzinger JP, Hardgrove C, Herkenhoff KE, Horgan B, Jaumann R, Johnson JR, Lemmon M, Paar G, Caballo-Perucha M, Gupta S, Traxler C, Preusker F, Rice MS, Robinson MS, Schmitz N, Sullivan R, Wolff MJ. The Mars 2020 Perseverance Rover Mast Camera Zoom (Mastcam-Z) Multispectral, Stereoscopic Imaging Investigation. SPACE SCIENCE REVIEWS 2021; 217:24. [PMID: 33612866 PMCID: PMC7883548 DOI: 10.1007/s11214-020-00755-x] [Citation(s) in RCA: 5] [Impact Index Per Article: 1.7] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/22/2020] [Accepted: 09/25/2020] [Indexed: 05/16/2023]
Abstract
Mastcam-Z is a multispectral, stereoscopic imaging investigation on the Mars 2020 mission's Perseverance rover. Mastcam-Z consists of a pair of focusable, 4:1 zoomable cameras that provide broadband red/green/blue and narrowband 400-1000 nm color imaging with fields of view from 25.6° × 19.2° (26 mm focal length at 283 μrad/pixel) to 6.2° × 4.6° (110 mm focal length at 67.4 μrad/pixel). The cameras can resolve (≥ 5 pixels) ∼0.7 mm features at 2 m and ∼3.3 cm features at 100 m distance. Mastcam-Z shares significant heritage with the Mastcam instruments on the Mars Science Laboratory Curiosity rover. Each Mastcam-Z camera consists of zoom, focus, and filter wheel mechanisms and a 1648 × 1214 pixel charge-coupled device detector and electronics. The two Mastcam-Z cameras are mounted with a 24.4 cm stereo baseline and 2.3° total toe-in on a camera plate ∼2 m above the surface on the rover's Remote Sensing Mast, which provides azimuth and elevation actuation. A separate digital electronics assembly inside the rover provides power, data processing and storage, and the interface to the rover computer. Primary and secondary Mastcam-Z calibration targets mounted on the rover top deck enable tactical reflectance calibration. Mastcam-Z multispectral, stereo, and panoramic images will be used to provide detailed morphology, topography, and geologic context along the rover's traverse; constrain mineralogic, photometric, and physical properties of surface materials; monitor and characterize atmospheric and astronomical phenomena; and document the rover's sample extraction and caching locations. Mastcam-Z images will also provide key engineering information to support sample selection and other rover driving and tool/instrument operations decisions.
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Affiliation(s)
| | | | | | - M. A. Ravine
- Malin Space Science Systems, Inc., San Diego, CA USA
| | | | | | - S. Brylow
- Malin Space Science Systems, Inc., San Diego, CA USA
| | | | | | | | | | | | | | - C. Tate
- Cornell Univ., Ithaca, NY USA
| | | | | | - E. Jensen
- Malin Space Science Systems, Inc., San Diego, CA USA
| | - K. Paris
- Arizona State Univ., Tempe, AZ USA
| | | | - C. Rojas
- Arizona State Univ., Tempe, AZ USA
| | | | | | | | - N. Cluff
- Arizona State Univ., Tempe, AZ USA
| | | | - B. Betts
- The Planetary Society, Pasadena, CA USA
| | | | - A. J. Coates
- Mullard Space Science Laboratory, Univ. College, London, UK
| | - A. Colaprete
- NASA/Ames Research Center, Moffett Field, CA USA
| | - K. S. Edgett
- Malin Space Science Systems, Inc., San Diego, CA USA
| | - B. L. Ehlmann
- JPL/Caltech, Pasadena, CA USA
- Caltech, Pasadena, CA USA
| | | | | | | | | | | | - R. Jaumann
- Inst. of Geological Sciences, Free University Berlin, Berlin, Germany
| | | | - M. Lemmon
- Space Science Inst., Boulder, CO USA
| | - G. Paar
- Joanneum Research, Graz, Austria
| | | | | | | | - F. Preusker
- DLR/German Aerospace Center, Berlin, Germany
| | - M. S. Rice
- Western Washington Univ., Bellingham, WA USA
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9
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Pla-García J, Rafkin SCR, Martinez GM, Vicente-Retortillo Á, Newman CE, Savijärvi H, de la Torre M, Rodriguez-Manfredi JA, Gómez F, Molina A, Viúdez-Moreiras D, Harri AM. Meteorological Predictions for Mars 2020 Perseverance Rover Landing Site at Jezero Crater. SPACE SCIENCE REVIEWS 2020; 216:148. [PMID: 33536691 PMCID: PMC7116669 DOI: 10.1007/s11214-020-00763-x] [Citation(s) in RCA: 4] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/16/2023]
Abstract
The Mars Regional Atmospheric Modeling System (MRAMS) and a nested simulation of the Mars Weather Research and Forecasting model (MarsWRF) are used to predict the local meteorological conditions at the Mars 2020 Perseverance rover landing site inside Jezero crater (Mars). These predictions are complemented with the COmplutense and MIchigan MArs Radiative Transfer model (COMIMART) and with the local Single Column Model (SCM) to further refine predictions of radiative forcing and the water cycle respectively. The primary objective is to facilitate interpretation of the meteorological measurements to be obtained by the Mars Environmental Dynamics Analyzer (MEDA) aboard the rover, but also to provide predictions of the meteorological phenomena and seasonal changes that might impact operations, from both a risk perspective and from the perspective of being better prepared to make certain measurements. A full diurnal cycle at four different seasons (Ls 0°, 90°, 180°, and 270°) is investigated. Air and ground temperatures, pressure, wind speed and direction, surface radiative fluxes and moisture data are modeled. The good agreement between observations and modeling in prior works [Pla-Garcia et al. in Icarus 280:103-113, 2016; Newman et al. in Icarus 291:203-231, 2017; Vicente-Retortillo et al. in Sci. Rep. 8(1):1-8, 2018; Savijarvi et al. in Icarus, 2020] provides confidence in utilizing these models results to predict the meteorological environment at Mars 2020 Perseverance rover landing site inside Jezero crater. The data returned by MEDA will determine the extent to which this confidence was justified.
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Affiliation(s)
- Jorge Pla-García
- Centro de Astrobiología (CSIC-INTA), Madrid, Spain
- Space Science Institute, Boulder, CO, USA
| | | | - G M Martinez
- Lunar and Planetary Institute, Houston, TX, USA
- University of Michigan, Ann Arbor, MI, USA
| | - Á Vicente-Retortillo
- Centro de Astrobiología (CSIC-INTA), Madrid, Spain
- University of Michigan, Ann Arbor, MI, USA
| | | | - H Savijärvi
- Institute for Atmospheric and Earth System Research/Physics, University of Helsinki, Finland
- Finnish Meteorological Institute, Helsinki, Finland
| | - M de la Torre
- Jet Propulsion Laboratory/CalTech, Pasadena, CA, USA
| | | | - F Gómez
- Centro de Astrobiología (CSIC-INTA), Madrid, Spain
| | - A Molina
- Centro de Astrobiología (CSIC-INTA), Madrid, Spain
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10
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Fraeman AA, Johnson JR, Arvidson RE, Rice MS, Wellington DF, Morris RV, Fox VK, Horgan BHN, Jacob SR, Salvatore MR, Sun VZ, Pinet P, Bell JF, Wiens RC, Vasavada AR. Synergistic Ground and Orbital Observations of Iron Oxides on Mt. Sharp and Vera Rubin Ridge. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2020; 125:e2019JE006294. [PMID: 33042722 PMCID: PMC7539960 DOI: 10.1029/2019je006294] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 11/26/2019] [Revised: 07/21/2020] [Accepted: 07/23/2020] [Indexed: 05/04/2023]
Abstract
Visible/short-wave infrared spectral data from the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) show absorptions attributed to hematite at Vera Rubin ridge (VRR), a topographic feature on northwest Mt. Sharp. The goals of this study are to determine why absorptions caused by ferric iron are strongly visible from orbit at VRR and to improve interpretation of CRISM data throughout lower Mt. Sharp. These goals are achieved by analyzing coordinated CRISM and in situ spectral data along the Curiosity Mars rover's traverse. VRR bedrock within areas that have the deepest ferric absorptions in CRISM data also has the deepest ferric absorptions measured in situ. This suggests strong ferric absorptions are visible from orbit at VRR because of the unique spectral properties of VRR bedrock. Dust and mixing with basaltic sand additionally inhibit the ability to measure ferric absorptions in bedrock stratigraphically below VRR from orbit. There are two implications of these findings: (1) Ferric absorptions in CRISM data initially dismissed as noise could be real, and ferric phases are more widespread in lower Mt. Sharp than previously reported. (2) Patches with the deepest ferric absorptions in CRISM data are, like VRR, reflective of deeper absorptions in the bedrock. One model to explain this spectral variability is late-stage diagenetic fluids that changed the grain size of ferric phases, deepening absorptions. Curiosity's experience highlights the strengths of using CRISM data for spectral absorptions and associated mineral detections and the caveats in using these data for geologic interpretations and strategic path planning tools.
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Affiliation(s)
- A. A. Fraeman
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - J. R. Johnson
- Johns Hopkins University Applied Physics LaboratoryLaurelMDUSA
| | - R. E. Arvidson
- Department of Earth and Planetary SciencesWashington UniversitySt. LouisMOUSA
| | - M. S. Rice
- Geology Department, Physics and Astronomy DepartmentWestern Washington UniversityBellinghamWAUSA
| | - D. F. Wellington
- School of Earth and Space ExplorationArizona State UniversityTempeAZUSA
| | | | - V. K. Fox
- Division of Geological and Planetary SciencesCalifornia Institute of TechnologyPasadenaCAUSA
| | - B. H. N. Horgan
- Department of Earth, Atmospheric, and Planetary SciencesPurdue UniversityWest LafayetteINUSA
| | - S. R. Jacob
- School of Earth and Space ExplorationArizona State UniversityTempeAZUSA
| | - M. R. Salvatore
- Department of Astronomy and Planetary ScienceNorthern Arizona UniversityFlagstaffAZUSA
| | - V. Z. Sun
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - P. Pinet
- Institut de Recherche en Astrophysique et PlanétologieUniversité de Toulouse, CNRS, UPS, CNESToulouseFrance
| | - J. F. Bell
- School of Earth and Space ExplorationArizona State UniversityTempeAZUSA
| | - R. C. Wiens
- Los Alamos National LaboratoryLos AlamosNMUSA
| | - A. R. Vasavada
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
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11
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Streeter PM, Lewis SR, Patel MR, Holmes JA, Kass DM. Surface Warming During the 2018/Mars Year 34 Global Dust Storm. GEOPHYSICAL RESEARCH LETTERS 2020; 47:e2019GL083936. [PMID: 32713983 PMCID: PMC7375149 DOI: 10.1029/2019gl083936] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 05/31/2019] [Revised: 08/29/2019] [Accepted: 09/02/2019] [Indexed: 06/11/2023]
Abstract
The impact of Mars's 2018 Global Dust Storm (GDS) on surface and near-surface air temperatures was investigated using an assimilation of Mars Climate Sounder observations. Rather than simply resulting in cooling everywhere from solar absorption (average surface radiative flux fell 26 W/m2), the globally averaged result was a 0.9-K surface warming. These diurnally averaged surface temperature changes had a novel, highly nonuniform spatial structure, with up to 16-K cooling/19-K warming. Net warming occurred in low thermal inertia regions, where rapid nighttime radiative cooling was compensated by increased longwave emission and scattering. This caused strong nightside warming, outweighing dayside cooling. The reduced surface-air temperature gradient closely coupled surface and air temperatures, even causing local dayside air warming. Results show good agreement with Mars Climate Sounder surface temperature retrievals. Comparisons with the 2001 GDS and free-running simulations show that GDS spatial structure is crucial in determining global surface temperature effects.
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Affiliation(s)
| | | | - Manish R. Patel
- School of Physical SciencesThe Open UniversityMilton KeynesUK
- Space Science and Technology DepartmentScience and Technology Facilities Council, Rutherford Appleton LaboratoryDidcotUK
| | - James A. Holmes
- School of Physical SciencesThe Open UniversityMilton KeynesUK
| | - David M. Kass
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
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12
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Fedorova AA, Montmessin F, Korablev O, Luginin M, Trokhimovskiy A, Belyaev DA, Ignatiev NI, Lefèvre F, Alday J, Irwin PGJ, Olsen KS, Bertaux JL, Millour E, Määttänen A, Shakun A, Grigoriev AV, Patrakeev A, Korsa S, Kokonkov N, Baggio L, Forget F, Wilson CF. Stormy water on Mars: The distribution and saturation of atmospheric water during the dusty season. Science 2020; 367:297-300. [PMID: 31919130 DOI: 10.1126/science.aay9522] [Citation(s) in RCA: 73] [Impact Index Per Article: 18.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 08/01/2019] [Accepted: 12/18/2019] [Indexed: 11/02/2022]
Abstract
The loss of water from Mars to space is thought to result from the transport of water to the upper atmosphere, where it is dissociated to hydrogen and escapes the planet. Recent observations have suggested large, rapid seasonal intrusions of water into the upper atmosphere, boosting the hydrogen abundance. We use the Atmospheric Chemistry Suite on the ExoMars Trace Gas Orbiter to characterize the water distribution by altitude. Water profiles during the 2018-2019 southern spring and summer stormy seasons show that high-altitude water is preferentially supplied close to perihelion, and supersaturation occurs even when clouds are present. This implies that the potential for water to escape from Mars is higher than previously thought.
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Affiliation(s)
- Anna A Fedorova
- Space Research Institute of the Russian Academy of Sciences (IKI RAS), Moscow, Russia.
| | - Franck Montmessin
- Laboratoire Atmosphères Milieux Observations Spatiales (LATMOS), Université Paris-Saclay, Sorbonne Université, Centre National de la Recherche Scientifique, Guyancourt, France
| | - Oleg Korablev
- Space Research Institute of the Russian Academy of Sciences (IKI RAS), Moscow, Russia
| | - Mikhail Luginin
- Space Research Institute of the Russian Academy of Sciences (IKI RAS), Moscow, Russia
| | | | - Denis A Belyaev
- Space Research Institute of the Russian Academy of Sciences (IKI RAS), Moscow, Russia
| | - Nikolay I Ignatiev
- Space Research Institute of the Russian Academy of Sciences (IKI RAS), Moscow, Russia
| | - Franck Lefèvre
- Laboratoire Atmosphères Milieux Observations Spatiales (LATMOS), Université Paris-Saclay, Sorbonne Université, Centre National de la Recherche Scientifique, Guyancourt, France
| | - Juan Alday
- Physics Department, Oxford University, Oxford, UK
| | | | - Kevin S Olsen
- Laboratoire Atmosphères Milieux Observations Spatiales (LATMOS), Université Paris-Saclay, Sorbonne Université, Centre National de la Recherche Scientifique, Guyancourt, France.,Physics Department, Oxford University, Oxford, UK
| | - Jean-Loup Bertaux
- Space Research Institute of the Russian Academy of Sciences (IKI RAS), Moscow, Russia.,Laboratoire Atmosphères Milieux Observations Spatiales (LATMOS), Université Paris-Saclay, Sorbonne Université, Centre National de la Recherche Scientifique, Guyancourt, France
| | - Ehouarn Millour
- Laboratoire de Météorologie Dynamique, Sorbonne Université, Centre National de la Recherche Scientifique, Jussieu, Paris, France
| | - Anni Määttänen
- Laboratoire Atmosphères Milieux Observations Spatiales (LATMOS), Université Paris-Saclay, Sorbonne Université, Centre National de la Recherche Scientifique, Guyancourt, France
| | - Alexey Shakun
- Space Research Institute of the Russian Academy of Sciences (IKI RAS), Moscow, Russia
| | - Alexey V Grigoriev
- Space Research Institute of the Russian Academy of Sciences (IKI RAS), Moscow, Russia.,Research School of Astronomy and Astrophysics and Advanced Instrumentation and Technology Centre at Mount Stromlo Observatory, Australian National University, Canberra, Australia
| | - Andrey Patrakeev
- Space Research Institute of the Russian Academy of Sciences (IKI RAS), Moscow, Russia
| | - Svyatoslav Korsa
- Space Research Institute of the Russian Academy of Sciences (IKI RAS), Moscow, Russia
| | - Nikita Kokonkov
- Space Research Institute of the Russian Academy of Sciences (IKI RAS), Moscow, Russia
| | - Lucio Baggio
- Laboratoire Atmosphères Milieux Observations Spatiales (LATMOS), Université Paris-Saclay, Sorbonne Université, Centre National de la Recherche Scientifique, Guyancourt, France
| | - Francois Forget
- Laboratoire de Météorologie Dynamique, Sorbonne Université, Centre National de la Recherche Scientifique, Jussieu, Paris, France
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13
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The Mars Regional Atmospheric Modeling System (MRAMS): Current Status and Future Directions. ATMOSPHERE 2019. [DOI: 10.3390/atmos10120747] [Citation(s) in RCA: 12] [Impact Index Per Article: 2.4] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 01/30/2023]
Abstract
The Mars Regional Atmospheric Modeling System (MRAMS) is closing in on two decades of use as a tool to investigate mesoscale and microscale circulations and dynamics in the atmosphere of Mars. Over this period of time, there have been numerous improvements and additions to the model dynamical core, physical parameterizations, and framework. At the same time, the application of the model to Mars (and related code for other planets) has taught many lessons about limitations and cautions that should be exercised. The current state of MRAMS is described along with a review of prior studies and findings utilizing the model. Where appropriate, lessons learned are provided to help guide future users and aid in the design and interpretation of numerical experiments. The paper concludes with a discussion of future MRAMS development plans.
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14
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Heavens NG. An Observational Overview of Dusty Deep Convection in Martian Dust Storms. JOURNAL OF THE ATMOSPHERIC SCIENCES 2019; 76:3299-3326. [PMID: 32848258 PMCID: PMC7446947 DOI: 10.1175/jas-d-19-0042.1] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/11/2023]
Abstract
Deep convection, as used in meteorology, refers to the rapid ascent of air parcels in the Earth's troposphere driven by the buoyancy generated by phase change in water. Deep convection undergirds some of the Earth's most important and violent weather phenomena and is responsible for many aspects of the observed distribution of energy, momentum, and constituents (particularly water) in the Earth's atmosphere. Deep convection driven by buoyancy generated by the radiative heating of atmospheric dust may be similarly important in the atmosphere of Mars but lacks a systematic description. Here we propose a comprehensive framework for this phenomenon of dusty deep convection (DDC) that is supported by energetic calculations and observations of the vertical dust distribution and exemplary dusty deep convective structures within local, regional, and global dust storm activity. In this framework, DDC is distinct from a spectrum of weaker dusty convective activity because DDC originates from pre-existing or concurrently forming mesoscale circulations that generate high surface dust fluxes, oppose large-scale horizontal advective-diffusive processes, and are thus able to maintain higher dust concentrations than typically simulated. DDC takes two distinctive forms. Mesoscale circulations that form near Mars's highest volcanoes in dust storms of all scales can transport dust to the base of the upper atmosphere in as little as two hours. In the second distinctive form, mesoscale circulations at low elevations within regional and global dust storm activity generate freely convecting streamers of dust that are sheared into the middle atmosphere over the diurnal cycle.
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Affiliation(s)
- Nicholas G. Heavens
- Department of Atmospheric and Planetary Sciences, Hampton University, Hampton, Virginia; Space Science Institute, Boulder, Colorado
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15
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Vandaele AC, Korablev O, Daerden F, Aoki S, Thomas IR, Altieri F, López-Valverde M, Villanueva G, Liuzzi G, Smith MD, Erwin JT, Trompet L, Fedorova AA, Montmessin F, Trokhimovskiy A, Belyaev DA, Ignatiev NI, Luginin M, Olsen KS, Baggio L, Alday J, Bertaux JL, Betsis D, Bolsée D, Clancy RT, Cloutis E, Depiesse C, Funke B, Garcia-Comas M, Gérard JC, Giuranna M, Gonzalez-Galindo F, Grigoriev AV, Ivanov YS, Kaminski J, Karatekin O, Lefèvre F, Lewis S, López-Puertas M, Mahieux A, Maslov I, Mason J, Mumma MJ, Neary L, Neefs E, Patrakeev A, Patsaev D, Ristic B, Robert S, Schmidt F, Shakun A, Teanby NA, Viscardy S, Willame Y, Whiteway J, Wilquet V, Wolff MJ, Bellucci G, Patel MR, López-Moreno JJ, Forget F, Wilson CF, Svedhem H, Vago JL, Rodionov D. Martian dust storm impact on atmospheric H 2O and D/H observed by ExoMars Trace Gas Orbiter. Nature 2019; 568:521-525. [PMID: 30971830 DOI: 10.1038/s41586-019-1097-3] [Citation(s) in RCA: 82] [Impact Index Per Article: 16.4] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 11/16/2018] [Accepted: 03/14/2019] [Indexed: 11/09/2022]
Abstract
Global dust storms on Mars are rare1,2 but can affect the Martian atmosphere for several months. They can cause changes in atmospheric dynamics and inflation of the atmosphere3, primarily owing to solar heating of the dust3. In turn, changes in atmospheric dynamics can affect the distribution of atmospheric water vapour, with potential implications for the atmospheric photochemistry and climate on Mars4. Recent observations of the water vapour abundance in the Martian atmosphere during dust storm conditions revealed a high-altitude increase in atmospheric water vapour that was more pronounced at high northern latitudes5,6, as well as a decrease in the water column at low latitudes7,8. Here we present concurrent, high-resolution measurements of dust, water and semiheavy water (HDO) at the onset of a global dust storm, obtained by the NOMAD and ACS instruments onboard the ExoMars Trace Gas Orbiter. We report the vertical distribution of the HDO/H2O ratio (D/H) from the planetary boundary layer up to an altitude of 80 kilometres. Our findings suggest that before the onset of the dust storm, HDO abundances were reduced to levels below detectability at altitudes above 40 kilometres. This decrease in HDO coincided with the presence of water-ice clouds. During the storm, an increase in the abundance of H2O and HDO was observed at altitudes between 40 and 80 kilometres. We propose that these increased abundances may be the result of warmer temperatures during the dust storm causing stronger atmospheric circulation and preventing ice cloud formation, which may confine water vapour to lower altitudes through gravitational fall and subsequent sublimation of ice crystals3. The observed changes in H2O and HDO abundance occurred within a few days during the development of the dust storm, suggesting a fast impact of dust storms on the Martian atmosphere.
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Affiliation(s)
| | - Oleg Korablev
- Space Research Institute (IKI), Russian Academy of Sciences (RAS), Moscow, Russia
| | - Frank Daerden
- Royal Belgian Institute for Space Aeronomy (IASB-BIRA), Brussels, Belgium
| | - Shohei Aoki
- Royal Belgian Institute for Space Aeronomy (IASB-BIRA), Brussels, Belgium
| | - Ian R Thomas
- Royal Belgian Institute for Space Aeronomy (IASB-BIRA), Brussels, Belgium
| | - Francesca Altieri
- Istituto di Astrofisica e Planetologia Spaziali (IAPS/INAF), Rome, Italy
| | - Miguel López-Valverde
- Instituto de Astrofìsica de Andalucia (IAA), Consejo Superior de Investigaciones Científicas (CSIC), Granada, Spain
| | | | | | | | - Justin T Erwin
- Royal Belgian Institute for Space Aeronomy (IASB-BIRA), Brussels, Belgium
| | - Loïc Trompet
- Royal Belgian Institute for Space Aeronomy (IASB-BIRA), Brussels, Belgium
| | - Anna A Fedorova
- Space Research Institute (IKI), Russian Academy of Sciences (RAS), Moscow, Russia
| | - Franck Montmessin
- Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), UVSQ Université Paris-Saclay, Sorbonne Université, CNRS, Paris, France
| | | | - Denis A Belyaev
- Space Research Institute (IKI), Russian Academy of Sciences (RAS), Moscow, Russia
| | - Nikolay I Ignatiev
- Space Research Institute (IKI), Russian Academy of Sciences (RAS), Moscow, Russia
| | - Mikhail Luginin
- Space Research Institute (IKI), Russian Academy of Sciences (RAS), Moscow, Russia
| | - Kevin S Olsen
- Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), UVSQ Université Paris-Saclay, Sorbonne Université, CNRS, Paris, France
| | - Lucio Baggio
- Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), UVSQ Université Paris-Saclay, Sorbonne Université, CNRS, Paris, France
| | - Juan Alday
- Department of Physics, Oxford University, Oxford, UK
| | - Jean-Loup Bertaux
- Space Research Institute (IKI), Russian Academy of Sciences (RAS), Moscow, Russia.,Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), UVSQ Université Paris-Saclay, Sorbonne Université, CNRS, Paris, France
| | - Daria Betsis
- Space Research Institute (IKI), Russian Academy of Sciences (RAS), Moscow, Russia
| | - David Bolsée
- Royal Belgian Institute for Space Aeronomy (IASB-BIRA), Brussels, Belgium
| | | | - Edward Cloutis
- Department of Geography, University of Winnipeg, Winnipeg, Manitoba, Canada
| | - Cédric Depiesse
- Royal Belgian Institute for Space Aeronomy (IASB-BIRA), Brussels, Belgium
| | - Bernd Funke
- Instituto de Astrofìsica de Andalucia (IAA), Consejo Superior de Investigaciones Científicas (CSIC), Granada, Spain
| | - Maia Garcia-Comas
- Instituto de Astrofìsica de Andalucia (IAA), Consejo Superior de Investigaciones Científicas (CSIC), Granada, Spain
| | - Jean-Claude Gérard
- Laboratory for Planetary and Atmospheric Physics (LPAP), University of Liège, Liège, Belgium
| | - Marco Giuranna
- Istituto di Astrofisica e Planetologia Spaziali (IAPS/INAF), Rome, Italy
| | - Francisco Gonzalez-Galindo
- Instituto de Astrofìsica de Andalucia (IAA), Consejo Superior de Investigaciones Científicas (CSIC), Granada, Spain
| | - Alexey V Grigoriev
- Space Research Institute (IKI), Russian Academy of Sciences (RAS), Moscow, Russia
| | - Yuriy S Ivanov
- Main Astronomical Observatory (MAO), National Academy of Sciences of Ukraine, Kiev, Ukraine
| | - Jacek Kaminski
- Institute of Geophysics, Polish Academy of Sciences, Warsaw, Poland
| | | | - Franck Lefèvre
- Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), UVSQ Université Paris-Saclay, Sorbonne Université, CNRS, Paris, France
| | - Stephen Lewis
- School of Physical Sciences, The Open University, Milton Keynes, UK
| | - Manuel López-Puertas
- Instituto de Astrofìsica de Andalucia (IAA), Consejo Superior de Investigaciones Científicas (CSIC), Granada, Spain
| | - Arnaud Mahieux
- Royal Belgian Institute for Space Aeronomy (IASB-BIRA), Brussels, Belgium
| | - Igor Maslov
- Space Research Institute (IKI), Russian Academy of Sciences (RAS), Moscow, Russia
| | - Jon Mason
- School of Physical Sciences, The Open University, Milton Keynes, UK
| | | | - Lori Neary
- Royal Belgian Institute for Space Aeronomy (IASB-BIRA), Brussels, Belgium
| | - Eddy Neefs
- Royal Belgian Institute for Space Aeronomy (IASB-BIRA), Brussels, Belgium
| | - Andrey Patrakeev
- Space Research Institute (IKI), Russian Academy of Sciences (RAS), Moscow, Russia
| | - Dmitry Patsaev
- Space Research Institute (IKI), Russian Academy of Sciences (RAS), Moscow, Russia
| | - Bojan Ristic
- Royal Belgian Institute for Space Aeronomy (IASB-BIRA), Brussels, Belgium
| | - Séverine Robert
- Royal Belgian Institute for Space Aeronomy (IASB-BIRA), Brussels, Belgium
| | - Frédéric Schmidt
- Geosciences Paris Sud (GEOPS), Université Paris Sud, Orsay, France
| | - Alexey Shakun
- Space Research Institute (IKI), Russian Academy of Sciences (RAS), Moscow, Russia
| | | | - Sébastien Viscardy
- Royal Belgian Institute for Space Aeronomy (IASB-BIRA), Brussels, Belgium
| | - Yannick Willame
- Royal Belgian Institute for Space Aeronomy (IASB-BIRA), Brussels, Belgium
| | - James Whiteway
- Centre for Research in Earth and Space Science, York University, Toronto, Ontario, Canada
| | - Valérie Wilquet
- Royal Belgian Institute for Space Aeronomy (IASB-BIRA), Brussels, Belgium
| | | | - Giancarlo Bellucci
- Istituto di Astrofisica e Planetologia Spaziali (IAPS/INAF), Rome, Italy
| | - Manish R Patel
- School of Physical Sciences, The Open University, Milton Keynes, UK
| | - Jose-Juan López-Moreno
- Instituto de Astrofìsica de Andalucia (IAA), Consejo Superior de Investigaciones Científicas (CSIC), Granada, Spain
| | - François Forget
- Laboratoire de Météorologie Dynamique (LMD), CNRS Jussieu, Paris, France
| | | | - Håkan Svedhem
- European Space Research and Technology Centre (ESTEC), ESA, Noordwijk, The Netherlands
| | - Jorge L Vago
- European Space Research and Technology Centre (ESTEC), ESA, Noordwijk, The Netherlands
| | - Daniel Rodionov
- Space Research Institute (IKI), Russian Academy of Sciences (RAS), Moscow, Russia
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16
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Ito G, Mishchenko MI, Glotch TD. Radiative-transfer modeling of spectra of planetary regoliths using cluster-based dense packing modifications. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2018; 123:1203-1220. [PMID: 30319931 PMCID: PMC6178094 DOI: 10.1029/2018je005532] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 01/11/2018] [Accepted: 03/30/2018] [Indexed: 06/08/2023]
Abstract
In remote sensing of planetary bodies, the development of analysis techniques that lead to quantitative interpretations of datasets has relatively been deficient compared to the wealth of acquired data, especially in the case of regoliths with particle sizes on the order of the probing wavelength. Radiative transfer theory has often been applied to the study of densely packed particulate media like planetary regoliths, but with difficulty; here we continue to improve theoretical modeling of spectra of densely packed particulate media. We use the superposition T-matrix method to compute the scattering properties of an elementary volume entering the radiative transfer equation by modeling it as a cluster of particles and thereby capture the near-field effects important for dense packing. Then, these scattering parameters are modified with the static structure factor correction to suppress the irrelevant far-field diffraction peak rendered by the T-matrix procedure. Using the corrected single- scattering parameters, reflectance (and emissivity) is computed via the invariant-imbedding solution to the scalar radiative transfer equation. We modeled the emissivity spectrum of the 3.3 μm particle size fraction of enstatite, representing a common regolith component, in the mid-infrared (~5 - 50 μm). The use of the static structure factor correction coupled with the superposition T-matrix method produced better agreement with the corresponding laboratory spectrum than the sole use of the T-matrix method, particularly for volume scattering wavelengths (transparency features). This work demonstrates the importance of proper treatment of the packing effects when modeling semi-infinite densely packed particulate media using finite, cluster-based light scattering models.
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Affiliation(s)
- Gen Ito
- Stony Brook University, Department of Geosciences, Stony Brook, NY, USA
- NASA Goddard Institute for Space Studies, New York, NY, USA
| | | | - Timothy D. Glotch
- Stony Brook University, Department of Geosciences, Stony Brook, NY, USA
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17
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Ranjan S, Wordsworth R, Sasselov DD. Atmospheric Constraints on the Surface UV Environment of Mars at 3.9 Ga Relevant to Prebiotic Chemistry. ASTROBIOLOGY 2017; 17:687-708. [PMID: 28537771 DOI: 10.1089/ast.2016.1596] [Citation(s) in RCA: 5] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/07/2023]
Abstract
Recent findings suggest that Mars may have been a clement environment for the emergence of life and may even have compared favorably to Earth in this regard. These findings have revived interest in the hypothesis that prebiotically important molecules or even nascent life may have formed on Mars and been transferred to Earth. UV light plays a key role in prebiotic chemistry. Characterizing the early martian surface UV environment is key to understanding how Mars compares to Earth as a venue for prebiotic chemistry. Here, we present two-stream, multilayer calculations of the UV surface radiance on Mars at 3.9 Ga to constrain the surface UV environment as a function of atmospheric state. We explore a wide range of atmospheric pressures, temperatures, and compositions that correspond to the diversity of martian atmospheric states consistent with available constraints. We include the effects of clouds and dust. We calculate dose rates to quantify the effect of different atmospheric states on UV-sensitive prebiotic chemistry. We find that, for normative clear-sky CO2-H2O atmospheres, the UV environment on young Mars is comparable to young Earth. This similarity is robust to moderate cloud cover; thick clouds (τcloud ≥ 100) are required to significantly affect the martian UV environment, because cloud absorption is degenerate with atmospheric CO2. On the other hand, absorption from SO2, H2S, and dust is nondegenerate with CO2, meaning that, if these constituents build up to significant levels, surface UV fluence can be suppressed. These absorbers have spectrally variable absorption, meaning that their presence affects prebiotic pathways in different ways. In particular, high SO2 environments may admit UV fluence that favors pathways conducive to abiogenesis over pathways unfavorable to it. However, better measurements of the spectral quantum yields of these pathways are required to evaluate this hypothesis definitively. Key Words: Radiative transfer-Origin of life-Mars-UV radiation-Prebiotic chemistry. Astrobiology 17, 687-708.
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Affiliation(s)
- Sukrit Ranjan
- 1 Harvard-Smithsonian Center for Astrophysics , Cambridge, Massachusetts
| | - Robin Wordsworth
- 2 Harvard Paulson School of Engineering and Applied Sciences, Harvard University , Cambridge, Massachusetts
- 3 Department of Earth and Planetary Sciences, Harvard University , Cambridge, Massachusetts
| | - Dimitar D Sasselov
- 1 Harvard-Smithsonian Center for Astrophysics , Cambridge, Massachusetts
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18
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Heavens NG. The Reflectivity of Mars at 1064 nm: Derivation from Mars Orbiter Laser Altimeter Data and Application to Climatology and Meteorology. ICARUS 2017; 289:1-21. [PMID: 32905474 PMCID: PMC7473108 DOI: 10.1016/j.icarus.2017.01.032] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/11/2023]
Abstract
The Mars Orbiter Laser Altimeter (MOLA) on board Mars Global Surveyor (MGS) made > 108 measurements of the reflectivity of Mars at 1064 nm (R 1064) by both active sounding and passive radiometry. Past studies of R 1064 neglected the effects of atmospheric opacity and viewing geometry on both active and passive measurements and also identified a potential calibration issue with passive radiometry. Therefore, as yet, there exists no acceptable reference R 1064 to derive a column opacity product for atmospheric studies and planning future orbital lidar observations. Here, such a reference R 1064 is derived by seeking R 1064 M , N : a Minnaert-corrected normal albedo under clear conditions and assuming minimal phase angle dependence. Over darker surfaces, R 1064 M , N and the absolute level of atmospheric opacity were estimated from active sounding. Over all surfaces, the opacity derived from active sounding was used to exclude passive radiometry measurements made under opaque conditions and estimate R 1064 M , N . These latter estimates then were re-calibrated by comparison with RM,N derived from Hubble Space Telescope (HST) observations over areas of approximately uniform reflectivity. Estimates of R 1064 M , N from re-calibrated passive radiometry typically agree with HST observations within 10 %. The resulting R 1064 M , N is then used to derive and quantify the uncertainties of a column opacity product, which can be applied to meteorological and climatological studies of Mars, particularly to detect and measure mesoscale cloud/aerosol structures.
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Affiliation(s)
- N G Heavens
- Department of Atmospheric and Planetary Sciences, Hampton University, 23 E. Tyler St., Hampton, Virginia, 23669
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19
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Read PL, Lewis SR, Mulholland DP. The physics of Martian weather and climate: a review. REPORTS ON PROGRESS IN PHYSICS. PHYSICAL SOCIETY (GREAT BRITAIN) 2015; 78:125901. [PMID: 26534887 DOI: 10.1088/0034-4885/78/12/125901] [Citation(s) in RCA: 7] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/16/2023]
Abstract
The planet Mars hosts an atmosphere that is perhaps the closest in terms of its meteorology and climate to that of the Earth. But Mars differs from Earth in its greater distance from the Sun, its smaller size, its lack of liquid oceans and its thinner atmosphere, composed mainly of CO(2). These factors give Mars a rather different climate to that of the Earth. In this article we review various aspects of the martian climate system from a physicist's viewpoint, focusing on the processes that control the martian environment and comparing these with corresponding processes on Earth. These include the radiative and thermodynamical processes that determine the surface temperature and vertical structure of the atmosphere, the fluid dynamics of its atmospheric motions, and the key cycles of mineral dust and volatile transport. In many ways, the climate of Mars is as complicated and diverse as that of the Earth, with complex nonlinear feedbacks that affect its response to variations in external forcing. Recent work has shown that the martian climate is anything but static, but is almost certainly in a continual state of transient response to slowly varying insolation associated with cyclic variations in its orbit and rotation. We conclude with a discussion of the physical processes underlying these long- term climate variations on Mars, and an overview of some of the most intriguing outstanding problems that should be a focus for future observational and theoretical studies.
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Affiliation(s)
- P L Read
- Atmospheric, Oceanic & Planetary Physics, University of Oxford, Clarendon Laboratory, Parks Road, Oxford, OX1 3PU, UK
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20
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Kinch KM, Bell JF, Goetz W, Johnson JR, Joseph J, Madsen MB, Sohl-Dickstein J. Dust deposition on the decks of the Mars Exploration Rovers: 10 years of dust dynamics on the Panoramic Camera calibration targets. EARTH AND SPACE SCIENCE (HOBOKEN, N.J.) 2015; 2:144-172. [PMID: 27981072 PMCID: PMC5125412 DOI: 10.1002/2014ea000073] [Citation(s) in RCA: 5] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Received: 12/23/2014] [Revised: 03/09/2015] [Accepted: 03/26/2015] [Indexed: 05/13/2023]
Abstract
The Panoramic Cameras on NASA's Mars Exploration Rovers have each returned more than 17,000 images of their calibration targets. In order to make optimal use of this data set for reflectance calibration, a correction must be made for the presence of air fall dust. Here we present an improved dust correction procedure based on a two-layer scattering model, and we present a dust reflectance spectrum derived from long-term trends in the data set. The dust on the calibration targets appears brighter than dusty areas of the Martian surface. We derive detailed histories of dust deposition and removal revealing two distinct environments: At the Spirit landing site, half the year is dominated by dust deposition, the other half by dust removal, usually in brief, sharp events. At the Opportunity landing site the Martian year has a semiannual dust cycle with dust removal happening gradually throughout two removal seasons each year. The highest observed optical depth of settled dust on the calibration target is 1.5 on Spirit and 1.1 on Opportunity (at 601 nm). We derive a general prediction for dust deposition rates of 0.004 ± 0.001 in units of surface optical depth deposited per sol (Martian solar day) per unit atmospheric optical depth. We expect this procedure to lead to improved reflectance-calibration of the Panoramic Camera data set. In addition, it is easily adapted to similar data sets from other missions in order to deliver improved reflectance calibration as well as data on dust reflectance properties and deposition and removal history.
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Affiliation(s)
- Kjartan M Kinch
- Niels Bohr Institute University of Copenhagen Copenhagen Denmark
| | - James F Bell
- School of Earth and Space Exploration Arizona State University Phoenix Arizona USA
| | - Walter Goetz
- Max Planck Institute for Solar System Research Göttingen Germany
| | - Jeffrey R Johnson
- Applied Physics Laboratory Johns Hopkins University Laurel Maryland USA
| | - Jonathan Joseph
- Department of Astronomy Cornell University Ithaca New York USA
| | - Morten Bo Madsen
- Niels Bohr Institute University of Copenhagen Copenhagen Denmark
| | - Jascha Sohl-Dickstein
- Neural Dynamics and Computation Laboratory Stanford University Stanford California USA
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Liuzzi G, Masiello G, Serio C, Fonti S, Mancarella F, Roush TL. Simultaneous physical retrieval of Martian geophysical parameters using Thermal Emission Spectrometer spectra: the φ-MARS algorithm. APPLIED OPTICS 2015; 54:2334-2346. [PMID: 25968519 DOI: 10.1364/ao.54.002334] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 09/11/2014] [Accepted: 01/05/2015] [Indexed: 06/04/2023]
Abstract
In this paper, we present a new methodology for the simultaneous retrieval of surface and atmospheric parameters of Mars. The methodology is essentially based on similar codes implemented for high-resolution instruments looking at Earth, supported by a statistical retrieval procedure used to initialize the physical retrieval algorithm with a reliable first guess of the atmospheric parameters. The methodology has been customized for the Thermal Emission Spectrometer (TES), which is a low-resolution interferometer. However, with minor changes to the forward and inverse modules, it is applicable to any instrument looking at Mars, and with particular effectiveness to high-resolution instruments. The forward module is a monochromatic radiative transfer model with the capability to calculate analytical Jacobians of any desired geophysical parameter. In the present work, we describe the general methodology and its application to a large sample of TES spectra. Results are drawn for the case of surface temperature and emissivity, atmospheric temperature profile, water vapor, and dust and ice mixing ratios. Comparison with climate models and other TES data analyses show very good agreement and consistency.
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22
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Villanueva GL, Mumma MJ, Novak RE, Käufl HU, Hartogh P, Encrenaz T, Tokunaga A, Khayat A, Smith MD. Strong water isotopic anomalies in the martian atmosphere: probing current and ancient reservoirs. Science 2015; 348:218-21. [PMID: 25745065 DOI: 10.1126/science.aaa3630] [Citation(s) in RCA: 208] [Impact Index Per Article: 23.1] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 11/24/2014] [Accepted: 02/06/2015] [Indexed: 11/02/2022]
Abstract
We measured maps of atmospheric water (H2O) and its deuterated form (HDO) across the martian globe, showing strong isotopic anomalies and a significant high deuterium/hydrogen (D/H) enrichment indicative of great water loss. The maps sample the evolution of sublimation from the north polar cap, revealing that the released water has a representative D/H value enriched by a factor of about 7 relative to Earth's ocean [Vienna standard mean ocean water (VSMOW)]. Certain basins and orographic depressions show even higher enrichment, whereas high-altitude regions show much lower values (1 to 3 VSMOW). Our atmospheric maps indicate that water ice in the polar reservoirs is enriched in deuterium to at least 8 VSMOW, which would mean that early Mars (4.5 billion years ago) had a global equivalent water layer at least 137 meters deep.
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Affiliation(s)
- G L Villanueva
- NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA. Catholic University of America, Washington, DC 20064, USA.
| | - M J Mumma
- NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
| | - R E Novak
- Iona College, New Rochelle, NY 10801, USA
| | - H U Käufl
- European Southern Observatory, Munich, Germany
| | - P Hartogh
- Max Planck Institute for Solar System Research, Katlenburg-Lindau 37191, Germany
| | - T Encrenaz
- Observatoire de Paris-Meudon, Meudon 92195, France
| | - A Tokunaga
- University of Hawaii-Manoa, Honolulu, HI 96822, USA
| | - A Khayat
- University of Hawaii-Manoa, Honolulu, HI 96822, USA
| | - M D Smith
- NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
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Arvidson RE, Squyres SW, Bell JF, Catalano JG, Clark BC, Crumpler LS, de Souza PA, Fairen AG, Farrand WH, Fox VK, Gellert R, Ghosh A, Golombek MP, Grotzinger JP, Guinness EA, Herkenhoff KE, Jolliff BL, Knoll AH, Li R, McLennan SM, Ming DW, Mittlefehldt DW, Moore JM, Morris RV, Murchie SL, Parker TJ, Paulsen G, Rice JW, Ruff SW, Smith MD, Wolff MJ. Ancient Aqueous Environments at Endeavour Crater, Mars. Science 2014; 343:1248097. [DOI: 10.1126/science.1248097] [Citation(s) in RCA: 133] [Impact Index Per Article: 13.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
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Merikallio S, Nousiainen T, Kahnert M, Harri AM. Light scattering by the Martian dust analog, palagonite, modeled with ellipsoids. OPTICS EXPRESS 2013; 21:17972-17985. [PMID: 23938669 DOI: 10.1364/oe.21.017972] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/02/2023]
Abstract
We have investigated the suitability of the ellipsoidal model particles to mimic scattering by Martian dust particles by comparing simulations against laboratory data for palagonite, a Mars analog sample. By optimizing the shape distribution of ellipsoids, a very good match with a laboratory-measured scattering matrix was obtained. Even an equiprobable distribution of ellipsoids performed well. The asymmetry parameter and single-scattering albedo were found to depend on the assumed shape distribution as much as on the typical uncertainties associated with refractive indices and size, suggesting that shape is an important parameter that potentially influences remote retrievals of dust particle properties.
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Affiliation(s)
- S Merikallio
- Finnish Meteorological Institute, P.O. Box 503, 00101 Finland.
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Madeleine JB, Forget F, Millour E, Montabone L, Wolff MJ. Revisiting the radiative impact of dust on Mars using the LMD Global Climate Model. ACTA ACUST UNITED AC 2011. [DOI: 10.1029/2011je003855] [Citation(s) in RCA: 123] [Impact Index Per Article: 9.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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26
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Wiseman SM, Arvidson RE, Morris RV, Poulet F, Andrews-Hanna JC, Bishop JL, Murchie SL, Seelos FP, Des Marais D, Griffes JL. Spectral and stratigraphic mapping of hydrated sulfate and phyllosilicate-bearing deposits in northern Sinus Meridiani, Mars. ACTA ACUST UNITED AC 2010. [DOI: 10.1029/2009je003354] [Citation(s) in RCA: 58] [Impact Index Per Article: 4.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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27
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Cull S, Arvidson RE, Morris RV, Wolff M, Mellon MT, Lemmon MT. Seasonal ice cycle at the Mars Phoenix landing site: 2. Postlanding CRISM and ground observations. ACTA ACUST UNITED AC 2010. [DOI: 10.1029/2009je003410] [Citation(s) in RCA: 5] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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28
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Tamppari LK, Bass D, Cantor B, Daubar I, Dickinson C, Fisher D, Fujii K, Gunnlauggson HP, Hudson TL, Kass D, Kleinböhl A, Komguem L, Lemmon MT, Mellon M, Moores J, Pankine A, Pathak J, Searls M, Seelos F, Smith MD, Smrekar S, Taylor P, Holstein-Rathlou C, Weng W, Whiteway J, Wolff M. Phoenix and MRO coordinated atmospheric measurements. ACTA ACUST UNITED AC 2010. [DOI: 10.1029/2009je003415] [Citation(s) in RCA: 36] [Impact Index Per Article: 2.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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29
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Murchie SL, Seelos FP, Hash CD, Humm DC, Malaret E, McGovern JA, Choo TH, Seelos KD, Buczkowski DL, Morgan MF, Barnouin-Jha OS, Nair H, Taylor HW, Patterson GW, Harvel CA, Mustard JF, Arvidson RE, McGuire P, Smith MD, Wolff MJ, Titus TN, Bibring JP, Poulet F. Compact Reconnaissance Imaging Spectrometer for Mars investigation and data set from the Mars Reconnaissance Orbiter's primary science phase. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2009je003344] [Citation(s) in RCA: 146] [Impact Index Per Article: 9.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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