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Santalices D, Martínez-García M, Belmar J, Benito D, Briz S, Meléndez J, de Castro AJ. Calibration of a Dust Scattering Instrument Using Tomographic Techniques and Its Application to a Dust Sensor Instrument. SENSORS (BASEL, SWITZERLAND) 2023; 23:s23115036. [PMID: 37299764 DOI: 10.3390/s23115036] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 03/31/2023] [Revised: 05/19/2023] [Accepted: 05/21/2023] [Indexed: 06/12/2023]
Abstract
The characterization of suspended dust near the Martian surface is extremely relevant to understand the climate of Mars. In this frame, a Dust Sensor instrument, an infrared device designed to obtain the effective parameters of Martian dust using the scattering properties of the dust particles, was developed. The purpose of this article is to present a novel methodology to calculate, from experimental data, an instrumental function of the Dust Sensor that allows solving the direct problem and providing the signal that this instrument would provide given a distribution of particles. The experimental method is based on recording the signal measured when a Lambertian reflector is gradually introduced into the interaction volume at different distances from the detector and source and applying tomography techniques (inverse Radon transform) to obtain the image of a section of the interaction volume. This method provides a complete mapping of the interaction volume experimentally, which determines the Wf function. The method was applied to solve a specific case study. Among the advantages of this method, it should be noted that it avoids assumptions and idealizations of the dimensions of the volume of interaction and reduces the time required to carry out simulations.
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Affiliation(s)
- David Santalices
- LIR-Infrared Laboratory, Department of Physics, Universidad Carlos III de Madrid, 28911 Leganés, Spain
- Science Faculty, Universidad Nacional de Educación a Distancia (UNED), 28040 Madrid, Spain
| | - Mateo Martínez-García
- LIR-Infrared Laboratory, Department of Physics, Universidad Carlos III de Madrid, 28911 Leganés, Spain
| | - Jesús Belmar
- LIR-Infrared Laboratory, Department of Physics, Universidad Carlos III de Madrid, 28911 Leganés, Spain
| | - Daniel Benito
- LIR-Infrared Laboratory, Department of Physics, Universidad Carlos III de Madrid, 28911 Leganés, Spain
| | - Susana Briz
- LIR-Infrared Laboratory, Department of Physics, Universidad Carlos III de Madrid, 28911 Leganés, Spain
| | - Juan Meléndez
- LIR-Infrared Laboratory, Department of Physics, Universidad Carlos III de Madrid, 28911 Leganés, Spain
| | - Antonio J de Castro
- LIR-Infrared Laboratory, Department of Physics, Universidad Carlos III de Madrid, 28911 Leganés, Spain
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2
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Santalices D, de Castro AJ, Briz S. New Method to Calculate the Angular Weighting Function for a Scattering Instrument: Application to a Dust Sensor on Mars. SENSORS (BASEL, SWITZERLAND) 2022; 22:s22239216. [PMID: 36501918 PMCID: PMC9737661 DOI: 10.3390/s22239216] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Received: 09/23/2022] [Revised: 11/17/2022] [Accepted: 11/22/2022] [Indexed: 06/12/2023]
Abstract
Suspended dust above the Martian surface is an important element in Martian climatology. In the frame of the Exomars'22 mission, we developed a dust sensor instrument, designed to provide size parameters of dust particles suspended in Mars surface from the light scattered by the particles. Thus, to interpret the data of the dust sensor, we need a method to calculate the theoretical optical power dispersed by the particles and, therefore, the theoretical signal obtained by the instrument. This signal depends on the suspended particles and on the instrument configuration. In this paper, we present a new method to calculate the angular weighting function (Wf) for scattering sensors. Wf encompasses the scattering angles measured by the sensor and depends only on the instrument and not on the suspended particles. To calculate this Wf, we use fundamental radiometry principles and an appropriate coordinate system, where one coordinate is the scattering angle. The method is applied to the dust sensor instrument and compared with other methods. The comparison highlights the advantages of the proposed method since it avoids using an ideal sampling volume, preserves the radiometric meaning, and avoids instrument calibration. The effectiveness of the method makes it a valuable tool for the design of scattering instruments and also for the interpretation of their data.
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Affiliation(s)
- David Santalices
- LIR—Infrared Laboratory, Department of Physics, Universidad Carlos III de Madrid, 28911 Leganés, Spain
- Science Faculty, Universidad Nacional de Educación a Distancia (UNED), 28040 Madrid, Spain
| | - Antonio J. de Castro
- LIR—Infrared Laboratory, Department of Physics, Universidad Carlos III de Madrid, 28911 Leganés, Spain
| | - Susana Briz
- LIR—Infrared Laboratory, Department of Physics, Universidad Carlos III de Madrid, 28911 Leganés, Spain
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3
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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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4
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Rodriguez-Manfredi JA, de la Torre Juárez M, Alonso A, Apéstigue V, Arruego I, Atienza T, Banfield D, Boland J, Carrera MA, Castañer L, Ceballos J, Chen-Chen H, Cobos A, Conrad PG, Cordoba E, del Río-Gaztelurrutia T, de Vicente-Retortillo A, Domínguez-Pumar M, Espejo S, Fairen AG, Fernández-Palma A, Ferrándiz R, Ferri F, Fischer E, García-Manchado A, García-Villadangos M, Genzer M, Giménez S, Gómez-Elvira J, Gómez F, Guzewich SD, Harri AM, Hernández CD, Hieta M, Hueso R, Jaakonaho I, Jiménez JJ, Jiménez V, Larman A, Leiter R, Lepinette A, Lemmon MT, López G, Madsen SN, Mäkinen T, Marín M, Martín-Soler J, Martínez G, Molina A, Mora-Sotomayor L, Moreno-Álvarez JF, Navarro S, Newman CE, Ortega C, Parrondo MC, Peinado V, Peña A, Pérez-Grande I, Pérez-Hoyos S, Pla-García J, Polkko J, Postigo M, Prieto-Ballesteros O, Rafkin SCR, Ramos M, Richardson MI, Romeral J, Romero C, Runyon KD, Saiz-Lopez A, Sánchez-Lavega A, Sard I, Schofield JT, Sebastian E, Smith MD, Sullivan RJ, Tamppari LK, Thompson AD, Toledo D, Torrero F, Torres J, Urquí R, Velasco T, Viúdez-Moreiras D, Zurita S. The Mars Environmental Dynamics Analyzer, MEDA. A Suite of Environmental Sensors for the Mars 2020 Mission. SPACE SCIENCE REVIEWS 2021; 217:48. [PMID: 34776548 PMCID: PMC8550605 DOI: 10.1007/s11214-021-00816-9] [Citation(s) in RCA: 4] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Accepted: 03/08/2021] [Indexed: 05/16/2023]
Abstract
NASA's Mars 2020 (M2020) rover mission includes a suite of sensors to monitor current environmental conditions near the surface of Mars and to constrain bulk aerosol properties from changes in atmospheric radiation at the surface. The Mars Environmental Dynamics Analyzer (MEDA) consists of a set of meteorological sensors including wind sensor, a barometer, a relative humidity sensor, a set of 5 thermocouples to measure atmospheric temperature at ∼1.5 m and ∼0.5 m above the surface, a set of thermopiles to characterize the thermal IR brightness temperatures of the surface and the lower atmosphere. MEDA adds a radiation and dust sensor to monitor the optical atmospheric properties that can be used to infer bulk aerosol physical properties such as particle size distribution, non-sphericity, and concentration. The MEDA package and its scientific purpose are described in this document as well as how it responded to the calibration tests and how it helps prepare for the human exploration of Mars. A comparison is also presented to previous environmental monitoring payloads landed on Mars on the Viking, Pathfinder, Phoenix, MSL, and InSight spacecraft.
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Affiliation(s)
| | | | | | - V. Apéstigue
- Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain
| | - I. Arruego
- Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain
| | - T. Atienza
- Universidad Politécnica de Cataluña, Barcelona, Spain
| | - D. Banfield
- Cornell Center for Astrophysics and Planetary Science, Cornell University, Ithaca, NY USA
| | - J. Boland
- Jet Propulsion Laboratory/California Institute of Technology, Pasadena, CA USA
| | | | - L. Castañer
- Universidad Politécnica de Cataluña, Barcelona, Spain
| | - J. Ceballos
- Instituto de Microelectrónica de Sevilla (US-CSIC), Seville, Spain
| | - H. Chen-Chen
- Universidad del País Vasco (UPV/EHU), Bilbao, Spain
| | - A. Cobos
- CRISA-Airbus, Tres Cantos, Spain
| | | | - E. Cordoba
- Jet Propulsion Laboratory/California Institute of Technology, Pasadena, CA USA
| | | | | | | | - S. Espejo
- Instituto de Microelectrónica de Sevilla (US-CSIC), Seville, Spain
| | - A. G. Fairen
- Centro de Astrobiología (INTA-CSIC), Madrid, Spain
| | | | - R. Ferrándiz
- Centro de Astrobiología (INTA-CSIC), Madrid, Spain
| | - F. Ferri
- Università degli Studi di Padova, Padova, Italy
| | - E. Fischer
- University of Michigan, Ann Arbor, MI USA
| | | | | | - M. Genzer
- Finnish Meteorological Institute, Helsinki, Finland
| | - S. Giménez
- Centro de Astrobiología (INTA-CSIC), Madrid, Spain
| | - J. Gómez-Elvira
- Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain
| | - F. Gómez
- Centro de Astrobiología (INTA-CSIC), Madrid, Spain
| | | | - A.-M. Harri
- Finnish Meteorological Institute, Helsinki, Finland
| | - C. D. Hernández
- Jet Propulsion Laboratory/California Institute of Technology, Pasadena, CA USA
| | - M. Hieta
- Finnish Meteorological Institute, Helsinki, Finland
| | - R. Hueso
- Universidad del País Vasco (UPV/EHU), Bilbao, Spain
| | - I. Jaakonaho
- Finnish Meteorological Institute, Helsinki, Finland
| | - J. J. Jiménez
- Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain
| | - V. Jiménez
- Universidad Politécnica de Cataluña, Barcelona, Spain
| | - A. Larman
- Added-Value-Solutions, Elgoibar, Spain
| | - R. Leiter
- Jet Propulsion Laboratory/California Institute of Technology, Pasadena, CA USA
| | - A. Lepinette
- Centro de Astrobiología (INTA-CSIC), Madrid, Spain
| | | | - G. López
- Universidad Politécnica de Cataluña, Barcelona, Spain
| | - S. N. Madsen
- Jet Propulsion Laboratory/California Institute of Technology, Pasadena, CA USA
| | - T. Mäkinen
- Finnish Meteorological Institute, Helsinki, Finland
| | - M. Marín
- Centro de Astrobiología (INTA-CSIC), Madrid, Spain
| | | | - G. Martínez
- Lunar and Planetary Institute, Houston, TX USA
| | - A. Molina
- Centro de Astrobiología (INTA-CSIC), Madrid, Spain
| | | | | | - S. Navarro
- Centro de Astrobiología (INTA-CSIC), Madrid, Spain
| | | | - C. Ortega
- Added-Value-Solutions, Elgoibar, Spain
| | - M. C. Parrondo
- Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain
| | - V. Peinado
- Centro de Astrobiología (INTA-CSIC), Madrid, Spain
| | - A. Peña
- CRISA-Airbus, Tres Cantos, Spain
| | | | | | | | - J. Polkko
- Finnish Meteorological Institute, Helsinki, Finland
| | - M. Postigo
- Centro de Astrobiología (INTA-CSIC), Madrid, Spain
| | | | | | - M. Ramos
- Universidad de Alcalá, Alcalá de Henares, Spain
| | | | - J. Romeral
- Centro de Astrobiología (INTA-CSIC), Madrid, Spain
| | - C. Romero
- Centro de Astrobiología (INTA-CSIC), Madrid, Spain
| | | | - A. Saiz-Lopez
- Dept. of Atmospheric Chemistry and Climate, Institute of Physical Chemistry Rocasolano, CSIC, Madrid, Spain
| | | | - I. Sard
- Added-Value-Solutions, Elgoibar, Spain
| | - J. T. Schofield
- Jet Propulsion Laboratory/California Institute of Technology, Pasadena, CA USA
| | - E. Sebastian
- Centro de Astrobiología (INTA-CSIC), Madrid, Spain
| | - M. D. Smith
- NASA Goddard Space Flight Center, Greenbelt, MD USA
| | - R. J. Sullivan
- Cornell Center for Astrophysics and Planetary Science, Cornell University, Ithaca, NY USA
| | - L. K. Tamppari
- Jet Propulsion Laboratory/California Institute of Technology, Pasadena, CA USA
| | - A. D. Thompson
- Jet Propulsion Laboratory/California Institute of Technology, Pasadena, CA USA
| | - D. Toledo
- Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain
| | | | - J. Torres
- Centro de Astrobiología (INTA-CSIC), Madrid, Spain
| | - R. Urquí
- Centro de Astrobiología (INTA-CSIC), Madrid, Spain
| | | | | | - S. Zurita
- Centro de Astrobiología (INTA-CSIC), Madrid, Spain
| | - The MEDA team
- Centro de Astrobiología (INTA-CSIC), Madrid, Spain
- Jet Propulsion Laboratory/California Institute of Technology, Pasadena, CA USA
- CRISA-Airbus, Tres Cantos, Spain
- Instituto Nacional de Técnica Aeroespacial (INTA), Madrid, Spain
- Universidad Politécnica de Cataluña, Barcelona, Spain
- Cornell Center for Astrophysics and Planetary Science, Cornell University, Ithaca, NY USA
- Added-Value-Solutions, Elgoibar, Spain
- Instituto de Microelectrónica de Sevilla (US-CSIC), Seville, Spain
- Universidad del País Vasco (UPV/EHU), Bilbao, Spain
- Carnegie Institution, Washington, DC USA
- Università degli Studi di Padova, Padova, Italy
- University of Michigan, Ann Arbor, MI USA
- Finnish Meteorological Institute, Helsinki, Finland
- Space Science Institute, Boulder, CO USA
- Lunar and Planetary Institute, Houston, TX USA
- Aeolis Corporation, Sierra Madre, CA USA
- Universidad Politécnica de Madrid, Madrid, Spain
- Southwest Research Institute, Boulder, CO USA
- Universidad de Alcalá, Alcalá de Henares, Spain
- John Hopkins APL, Laurel, MD USA
- Dept. of Atmospheric Chemistry and Climate, Institute of Physical Chemistry Rocasolano, CSIC, Madrid, Spain
- NASA Goddard Space Flight Center, Greenbelt, MD USA
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5
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The Temporal Variation of Optical Depth in the Candidate Landing Area of China’s Mars Mission (Tianwen-1). REMOTE SENSING 2021. [DOI: 10.3390/rs13051029] [Citation(s) in RCA: 3] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/17/2022]
Abstract
The atmospheric dust is an important factor in the evolution of the Martian climate and has a major impact on the scientific exploration of the Martian lander or rover and its payload. This paper used remote sensing images to calculate atmospheric optical depth that characterizes the spatial distribution of the atmospheric dust of Mars. The optical depth calculated by the images of the High Resolution Imaging Science Experiment (HiRISE) in the inspection area of the Spirit rover had a similar temporal variation to the optical depth directly measured by the Spirit rover from the sunlight decay. We also used the HiRISE images to acquire the seasonal variation of optical depths in the candidate landing area of China’s Mars Mission (Tianwen-1). The results have shown that the seasonal pattern of the optical depth in the candidate landing area is consistent with the dust storm sequences in this area. After Tianwen-1 enters the orbit around Mars, the images collected by the Moderate Resolution Imaging Camera (MoRIC), and the High Resolution Imaging Camera (HiRIC) can be used to study the atmospheric optical depth in the candidate landing area, providing reference for the safe landing and operation of the lander and rover.
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6
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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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7
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Ding T, Deng Z, Hou X, Liu Y, Liu Y, Li M, Li M. Investigation on the simulation approach for Martian rarefied aeolian activities based on discrete element method. POWDER TECHNOL 2020. [DOI: 10.1016/j.powtec.2020.05.055] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/28/2022]
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8
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Moore CA, Moores JE, Newman CE, Lemmon MT, Guzewich SD, Battalio M. Vertical and Horizontal Heterogeneity of Atmospheric Dust Loading in Northern Gale Crater, Mars. ICARUS 2019; 329:197-206. [PMID: 31359883 PMCID: PMC6662233 DOI: 10.1016/j.icarus.2019.03.041] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/10/2023]
Abstract
This paper updates the record of atmospheric dust loading within northern Gale Crater, Mars, by providing line-of-sight extinction (LOS-Ext) measurements of the intervening dust between the rover and the crater rim. These measurements are derived from images taken with the Navigation Cameras (Navcam) onboard the Mars Science Laboratory (MSL) rover, Curiosity. The observations span 2.44 Mars years, from Mars Year (MY) 31 at a solar longitude (L S ) of 208° to t L S = 7° of MY34, sols 100 - 1701 of the MSL surface mission. This work examines the dataset for seasonal trends of the LOS-Ext in addition to horizontal variations and the vertical structure of LOS-Ext. The LOS-Ext has a repetitive pattern with a single peak in the latter half of the Mars year. The atmosphere in the crater is well mixed horizontally but not vertically as larger LOS-Ext is seen nearer the crater floor than at higher altitudes within the crater. The results allow a discussion on whether or not Gale Crater is a sink for atmospheric dust or a source of atmospheric dust in the current era.
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Affiliation(s)
- Casey A Moore
- York University, Centre for Research in Earth and Space Sciences (CRESS), 4700 Keele Street, Toronto ON M3J 1P3, Canada
| | - John E Moores
- York University, Centre for Research in Earth and Space Sciences (CRESS), 4700 Keele Street, Toronto ON M3J 1P3, Canada
| | | | - Mark T Lemmon
- Texas A&M University, Department of Atmospheric Sciences, MS 3150 College Station, Texas 77843, United States
| | - Scott D Guzewich
- NASA Goddard Space Flight Center, Greenbelt, MD 20771, United States
| | - Michael Battalio
- Texas A&M University, Department of Atmospheric Sciences, MS 3150 College Station, Texas 77843, United States
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9
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van Heereveld L, Merrison J, Nørnberg P, Finster K. Assessment of the Forward Contamination Risk of Mars by Clean Room Isolates from Space-Craft Assembly Facilities through Aeolian Transport - a Model Study. ORIGINS LIFE EVOL B 2017; 47:203-214. [PMID: 27461254 DOI: 10.1007/s11084-016-9515-0] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 02/01/2016] [Accepted: 06/13/2016] [Indexed: 10/21/2022]
Abstract
The increasing number of missions to Mars also increases the risk of forward contamination. Consequently there is a need for effective protocols to ensure efficient protection of the Martian environment against terrestrial microbiota. Despite the fact of constructing sophisticated clean rooms for spacecraft assembly a 100 % avoidance of contamination appears to be impossible. Recent surveys of these facilities have identified a significant number of microbes belonging to a variety of taxonomic groups that survive the harsh conditions of clean rooms. These microbes may have a strong contamination potential, which needs to be investigate to apply efficient decontamination treatments. In this study we propose a series of tests to evaluate the potential of clean room contaminants to survive the different steps involved in forward contamination. We used Staphylococcus xylosus as model organism to illustrate the different types of stress that potential contaminants will be subjected to on their way from the spacecraft onto the surface of Mars. Staphylococcus xylosus is associated with human skin and commonly found in clean rooms and could therefore contaminate the spacecraft as a result of human activity during the assembling process. The path the cell will take from the surface of the spacecraft onto the surface of Mars was split into steps representing different stresses that include desiccation, freezing, aeolian transport in a Martian-like atmosphere at Martian atmospheric pressure, and UV radiation climate. We assessed the surviving fraction of the cellular population after each step by determining the integrated metabolic activity of the survivor population by measuring their oxygen consumption rate. The largest fraction of the starting culture (around 70 %) was killed during desiccation, while freezing, Martian vacuum and short-term UV radiation only had a minor additional effect on the survivability of Staphylococcus xylosus. The study also included a simulation of atmospheric transport on Martian dust, which did not significantly alter the metabolic potential of the cells. The high survival potential of skin microbes, which are not among the most robust isolates, clearly underlines the necessity for efficient decontamination protocols and of adequate planetary protection measures. Thus we propose a series of tests to be included into the description of isolates from spacecraft assembly clean rooms in order to assess the forward contamination potential of the specific isolate and to categorize the risk level according to the organisms survival potential. We are aware that the tests that we propose do not exhaust the types of challenges that the microbes would meet on their way and therefore the series of tests is open to being extended.
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Affiliation(s)
- Luc van Heereveld
- Department of Bioscience, Aarhus University, Ny Munkegade 116, Building 1540, 8000, Aarhus C, Denmark
| | - Jonathan Merrison
- Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, Building 1520, 8000, Aarhus C, Denmark
| | - Per Nørnberg
- Department of Bioscience, Aarhus University, Ny Munkegade 116, Building 1540, 8000, Aarhus C, Denmark
| | - Kai Finster
- Department of Bioscience, Aarhus University, Ny Munkegade 116, Building 1540, 8000, Aarhus C, Denmark.
- Stellar Astrophysics Center, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, Building 1520, 8000, Aarhus C, Denmark.
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10
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Vandaele AC, Willame Y, Depiesse C, Thomas IR, Robert S, Bolsée D, Patel MR, Mason JP, Leese M, Lesschaeve S, Antoine P, Daerden F, Delanoye S, Drummond R, Neefs E, Ristic B, Lopez-Moreno JJ, Bellucci G, Team N. Optical and radiometric models of the NOMAD instrument part I: the UVIS channel. OPTICS EXPRESS 2015; 23:30028-30042. [PMID: 26698484 DOI: 10.1364/oe.23.030028] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/05/2023]
Abstract
The NOMAD instrument has been designed to best fulfil the science objectives of the ExoMars Trace Gas Orbiter mission that will be launched in 2016. The instrument is a combination of three channels that cover the UV, visible and IR spectral ranges and can perform solar occultation, nadir and limb observations. In this series of two papers, we present the optical models representing the three channels of the instrument and use them to determine signal to noise levels for different observation modes and Martian conditions. In this first part, we focus on the UVIS channel, which will sound the Martian atmosphere using nadir and solar occultation viewing modes, covering the 200-650nm spectral range. High SNR levels (>1000) can easily be reached for wavelengths higher than 300nm both in solar occultation and nadir modes when considering binning. Below 300nm SNR are lower primarily because of the lower signal and the impact of atmospheric absorption.
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11
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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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12
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Ehlers K, Chakrabarty R, Moosmüller H. Blue moons and Martian sunsets. APPLIED OPTICS 2014; 53:1808-1819. [PMID: 24663457 DOI: 10.1364/ao.53.001808] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 10/21/2013] [Accepted: 02/10/2014] [Indexed: 06/03/2023]
Abstract
The familiar yellow or orange disks of the moon and sun, especially when they are low in the sky, and brilliant red sunsets are a result of the selective extinction (scattering plus absorption) of blue light by atmospheric gas molecules and small aerosols, a phenomenon explainable using the Rayleigh scattering approximation. On rare occasions, dust or smoke aerosols can cause the extinction of red light to exceed that for blue, resulting in the disks of the sun and moon to appear as blue. Unlike Earth, the atmosphere of Mars is dominated by micron-size dust aerosols, and the sky during sunset takes on a bluish glow. Here we investigate the role of dust aerosols in the blue Martian sunsets and the occasional blue moons and suns on Earth. We use the Mie theory and the Debye series to calculate the wavelength-dependent optical properties of dust aerosols most commonly found on Mars. Our findings show that while wavelength selective extinction can cause the sun's disk to appear blue, the color of the glow surrounding the sun as observed from Mars is due to the dominance of near-forward scattering of blue light by dust particles and cannot be explained by a simple, Rayleigh-like selective extinction explanation.
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13
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UV and cold tolerance of a pigment-producing Antarctic Janthinobacterium sp. Ant5-2. Extremophiles 2013; 17:367-78. [DOI: 10.1007/s00792-013-0525-9] [Citation(s) in RCA: 17] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 12/13/2012] [Accepted: 01/31/2013] [Indexed: 10/27/2022]
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14
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Kok JF, Parteli EJR, Michaels TI, Karam DB. The physics of wind-blown sand and dust. REPORTS ON PROGRESS IN PHYSICS. PHYSICAL SOCIETY (GREAT BRITAIN) 2012; 75:106901. [PMID: 22982806 DOI: 10.1088/0034-4885/75/10/106901] [Citation(s) in RCA: 160] [Impact Index Per Article: 13.3] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/12/2023]
Abstract
The transport of sand and dust by wind is a potent erosional force, creates sand dunes and ripples, and loads the atmosphere with suspended dust aerosols. This paper presents an extensive review of the physics of wind-blown sand and dust on Earth and Mars. Specifically, we review the physics of aeolian saltation, the formation and development of sand dunes and ripples, the physics of dust aerosol emission, the weather phenomena that trigger dust storms, and the lifting of dust by dust devils and other small-scale vortices. We also discuss the physics of wind-blown sand and dune formation on Venus and Titan.
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Affiliation(s)
- Jasper F Kok
- Department of Earth and Atmospheric Sciences, Cornell University, Ithaca, NY, USA.
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15
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Moores JE, Schuerger AC. UV degradation of accreted organics on Mars: IDP longevity, surface reservoir of organics, and relevance to the detection of methane in the atmosphere. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/2012je004060] [Citation(s) in RCA: 36] [Impact Index Per Article: 3.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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16
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McGlynn IO, Fedo CM, McSween HY. Soil mineralogy at the Mars Exploration Rover landing sites: An assessment of the competing roles of physical sorting and chemical weathering. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/2011je003861] [Citation(s) in RCA: 39] [Impact Index Per Article: 3.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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17
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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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18
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Wolff MJ, Smith MD, Clancy RT, Arvidson R, Kahre M, Seelos F, Murchie S, Savijärvi H. Wavelength dependence of dust aerosol single scattering albedo as observed by the Compact Reconnaissance Imaging Spectrometer. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2009je003350] [Citation(s) in RCA: 159] [Impact Index Per Article: 10.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 01/25/2023]
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19
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Towner MC. Characteristics of large Martian dust devils using Mars Odyssey Thermal Emission Imaging System visual and infrared images. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2008je003220] [Citation(s) in RCA: 21] [Impact Index Per Article: 1.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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20
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Davy R, Taylor PA, Weng W, Li PY. A model of dust in the Martian lower atmosphere. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2008jd010481] [Citation(s) in RCA: 13] [Impact Index Per Article: 0.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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21
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Smith PH, Tamppari L, Arvidson RE, Bass D, Blaney D, Boynton W, Carswell A, Catling D, Clark B, Duck T, DeJong E, Fisher D, Goetz W, Gunnlaugsson P, Hecht M, Hipkin V, Hoffman J, Hviid S, Keller H, Kounaves S, Lange CF, Lemmon M, Madsen M, Malin M, Markiewicz W, Marshall J, McKay C, Mellon M, Michelangeli D, Ming D, Morris R, Renno N, Pike WT, Staufer U, Stoker C, Taylor P, Whiteway J, Young S, Zent A. Introduction to special section on the Phoenix Mission: Landing Site Characterization Experiments, Mission Overviews, and Expected Science. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2008je003083] [Citation(s) in RCA: 78] [Impact Index Per Article: 4.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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22
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Pathak J, Michelangeli DV, Komguem L, Whiteway J, Tamppari LK. Simulating Martian boundary layer water ice clouds and the lidar measurements for the Phoenix mission. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je002967] [Citation(s) in RCA: 13] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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23
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Sullivan R, Arvidson R, Bell JF, Gellert R, Golombek M, Greeley R, Herkenhoff K, Johnson J, Thompson S, Whelley P, Wray J. Wind-driven particle mobility on Mars: Insights from Mars Exploration Rover observations at “El Dorado” and surroundings at Gusev Crater. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2008je003101] [Citation(s) in RCA: 220] [Impact Index Per Article: 13.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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24
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Inada A, Garcia-Comas M, Altieri F, Gwinner K, Poulet F, Bellucci G, Keller HU, Markiewicz WJ, Richardson MI, Hoekzema N, Neukum G, Bibring JP. Dust haze in Valles Marineris observed by HRSC and OMEGA on board Mars Express. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je002893] [Citation(s) in RCA: 16] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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25
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Sharma R, Wyatt C, Zhang J, Mazumder MK, Calle CI, Mardesich N. Performance Analysis of Electrodynamic Self-Cleaning Transparent Films for its Applications to Mars and Lunar Missions. ACTA ACUST UNITED AC 2007. [DOI: 10.1109/07ias.2007.70] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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26
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Vincendon M, Langevin Y, Poulet F, Bibring JP, Gondet B. Recovery of surface reflectance spectra and evaluation of the optical depth of aerosols in the near-IR using a Monte Carlo approach: Application to the OMEGA observations of high-latitude regions of Mars. ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2006je002845] [Citation(s) in RCA: 61] [Impact Index Per Article: 3.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- M. Vincendon
- Institut d'Astrophysique Spatiale; CNRS/Université Paris Sud; Orsay France
| | - Y. Langevin
- Institut d'Astrophysique Spatiale; CNRS/Université Paris Sud; Orsay France
| | - F. Poulet
- Institut d'Astrophysique Spatiale; CNRS/Université Paris Sud; Orsay France
| | - J.-P. Bibring
- Institut d'Astrophysique Spatiale; CNRS/Université Paris Sud; Orsay France
| | - B. Gondet
- Institut d'Astrophysique Spatiale; CNRS/Université Paris Sud; Orsay France
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27
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Murchie S, Arvidson R, Bedini P, Beisser K, Bibring JP, Bishop J, Boldt J, Cavender P, Choo T, Clancy RT, Darlington EH, Des Marais D, Espiritu R, Fort D, Green R, Guinness E, Hayes J, Hash C, Heffernan K, Hemmler J, Heyler G, Humm D, Hutcheson J, Izenberg N, Lee R, Lees J, Lohr D, Malaret E, Martin T, McGovern JA, McGuire P, Morris R, Mustard J, Pelkey S, Rhodes E, Robinson M, Roush T, Schaefer E, Seagrave G, Seelos F, Silverglate P, Slavney S, Smith M, Shyong WJ, Strohbehn K, Taylor H, Thompson P, Tossman B, Wirzburger M, Wolff M. Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) on Mars Reconnaissance Orbiter (MRO). ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2006je002682] [Citation(s) in RCA: 666] [Impact Index Per Article: 39.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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28
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Kinch KM, Sohl-Dickstein J, Bell JF, Johnson JR, Goetz W, Landis GA. Dust deposition on the Mars Exploration Rover Panoramic Camera (Pancam) calibration targets. ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2006je002807] [Citation(s) in RCA: 57] [Impact Index Per Article: 3.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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29
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Abstract
Current proposals for the characterization of extrasolar terrestrial planets rest primarily on the use of spectroscopic techniques. While spectroscopy is effective in detecting the gaseous components of a planet's atmosphere, it provides no way of detecting the presence of liquid water, the defining characteristic of a habitable planet. In this paper, I investigate the potential of an alternative technique for characterizing the atmosphere of a planet using polarization. By looking for a polarization peak at the "primary rainbow" scattering angle, it is possible to detect the presence of liquid droplets in a planet's atmosphere and constrain the nature of the liquid through its refractive index. Single scattering calculations are presented to show that a well-defined rainbow scattering peak is present over the full range of likely cloud droplet sizes and clearly distinguishes the presence of liquid droplets from solid particles such as ice or dust. Rainbow scattering has been used in the past to determine the nature of the cloud droplets in the Venus atmosphere and by the POLarization and Directionality of Earth Reflectances (POLDER) instrument to distinguish between liquid and ice clouds in the Earth atmosphere. While the presence of liquid water clouds does not guarantee the presence of water at the surface, this technique could complement spectroscopic techniques for characterizing the atmospheres of potential habitable planets. The disk-integrated rainbow peak for Earth is estimated to be at a degree of polarization of 12.7% or 15.5% for two different cloud cover scenarios. The observation of this rainbow peak is shown to be feasible with the proposed Terrestrial Planet Finder Coronograph mission in similar total integration times to those required for spectroscopic characterization.
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Affiliation(s)
- Jeremy Bailey
- Australian Centre for Astrobiology, Macquarie University, Sydney, New South Wales, Australia.
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30
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Newsom HE, Crumpler LS, Reedy RC, Petersen MT, Newsom GC, Evans LG, Taylor GJ, Keller JM, Janes DM, Boynton WV, Kerry KE, Karunatillake S. Geochemistry of Martian soil and bedrock in mantled and less mantled terrains with gamma ray data from Mars Odyssey. ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2006je002680] [Citation(s) in RCA: 28] [Impact Index Per Article: 1.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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31
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Wolff MJ, Smith MD, Clancy RT, Spanovich N, Whitney BA, Lemmon MT, Bandfield JL, Banfield D, Ghosh A, Landis G, Christensen PR, Bell JF, Squyres SW. Constraints on dust aerosols from the Mars Exploration Rovers using MGS overflights and Mini-TES. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2006je002786] [Citation(s) in RCA: 132] [Impact Index Per Article: 7.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- M. J. Wolff
- Space Science Institute; Boulder Colorado USA
| | - M. D. Smith
- Goddard Space Flight Center; Greenbelt Maryland USA
| | | | - N. Spanovich
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | | | - M. T. Lemmon
- Department of Atmospheric Sciences; Texas A&M University; College Station Texas USA
| | - J. L. Bandfield
- Department of Geological Sciences; Arizona State University; Tempe Arizona USA
| | - D. Banfield
- Department of Astronomy; Cornell University; Ithaca New York USA
| | - A. Ghosh
- Department of Earth and Planetary Sciences; University of Tennessee; Knoxville Tennessee USA
| | - G. Landis
- Photovoltaics and Space Environment Branch; NASA John Glenn Research Center; Cleveland Ohio USA
| | - P. R. Christensen
- Department of Geological Sciences; Arizona State University; Tempe Arizona USA
| | - J. F. Bell
- Department of Astronomy; Cornell University; Ithaca New York USA
| | - S. W. Squyres
- Department of Astronomy; Cornell University; Ithaca New York USA
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32
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Golombek MP, Grant JA, Crumpler LS, Greeley R, Arvidson RE, Bell JF, Weitz CM, Sullivan R, Christensen PR, Soderblom LA, Squyres SW. Erosion rates at the Mars Exploration Rover landing sites and long-term climate change on Mars. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2006je002754] [Citation(s) in RCA: 181] [Impact Index Per Article: 10.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- M. P. Golombek
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - J. A. Grant
- Center for Earth and Planetary Studies, National Air and Space Museum; Smithsonian Institution; Washington, DC USA
| | - L. S. Crumpler
- New Mexico Museum of Natural History and Science; Albuquerque New Mexico USA
| | - R. Greeley
- Department of Geological Sciences; Arizona State University; Tempe Arizona USA
| | - R. E. Arvidson
- Department of Earth and Planetary Sciences; Washington University; St. Louis Missouri USA
| | - J. F. Bell
- Department of Astronomy; Cornell University; Ithaca New York USA
| | - C. M. Weitz
- Planetary Science Institute; Tucson Arizona USA
| | - R. Sullivan
- Department of Astronomy; Cornell University; Ithaca New York USA
| | - P. R. Christensen
- Department of Geological Sciences; Arizona State University; Tempe Arizona USA
| | | | - S. W. Squyres
- Department of Astronomy; Cornell University; Ithaca New York USA
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33
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Greeley R, Whelley PL, Arvidson RE, Cabrol NA, Foley DJ, Franklin BJ, Geissler PG, Golombek MP, Kuzmin RO, Landis GA, Lemmon MT, Neakrase LDV, Squyres SW, Thompson SD. Active dust devils in Gusev crater, Mars: Observations from the Mars Exploration Rover Spirit. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2006je002743] [Citation(s) in RCA: 114] [Impact Index Per Article: 6.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- Ronald Greeley
- School of Earth and Space Exploration; Arizona State University; Tempe Arizona USA
| | - Patrick L. Whelley
- School of Earth and Space Exploration; Arizona State University; Tempe Arizona USA
| | - Raymond E. Arvidson
- Department of Earth and Planetary Sciences; Washington University in St. Louis; St. Louis Missouri USA
| | | | - Daniel J. Foley
- School of Earth and Space Exploration; Arizona State University; Tempe Arizona USA
| | | | - Paul G. Geissler
- Astrogeology Program; U.S. Geological Survey; Flagstaff Arizona USA
| | | | | | | | - Mark T. Lemmon
- Department of Atmospheric Sciences; Texas A&M University; College Station Texas USA
| | - Lynn D. V. Neakrase
- School of Earth and Space Exploration; Arizona State University; Tempe Arizona USA
| | | | - Shane D. Thompson
- School of Earth and Space Exploration; Arizona State University; Tempe Arizona USA
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34
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Cantor BA, Kanak KM, Edgett KS. Mars Orbiter Camera observations of Martian dust devils and their tracks (September 1997 to January 2006) and evaluation of theoretical vortex models. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2006je002700] [Citation(s) in RCA: 116] [Impact Index Per Article: 6.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
| | - Katharine M. Kanak
- Cooperative Institute for Mesoscale Meteorological Studies; University of Oklahoma; Norman Oklahoma USA
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35
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Johnson JR, Sohl-Dickstein J, Grundy WM, Arvidson RE, Bell J, Christensen P, Graff T, Guinness EA, Kinch K, Morris R, Shepard MK. Radiative transfer modeling of dust-coated Pancam calibration target materials: Laboratory visible/near-infrared spectrogoniometry. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2005je002658] [Citation(s) in RCA: 24] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
| | | | | | - Raymond E. Arvidson
- Department of Earth and Planetary Sciences; Washington University; St. Louis Missouri USA
| | - James Bell
- Department of Astronomy; Cornell University; Ithaca New York USA
| | - Phil Christensen
- Department of Geological Sciences; Arizona State University; Tempe Arizona USA
| | - Trevor Graff
- Department of Geological Sciences; Arizona State University; Tempe Arizona USA
| | - Edward A. Guinness
- Department of Earth and Planetary Sciences; Washington University; St. Louis Missouri USA
| | - Kjartan Kinch
- Department of Astronomy; Cornell University; Ithaca New York USA
| | | | - Michael K. Shepard
- Department of Geography and Geosciences; Bloomsburg University; Bloomsburg Pennsylvania USA
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36
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Rannou P, Perrier S, Bertaux JL, Montmessin F, Korablev O, Rébérac A. Dust and cloud detection at the Mars limb with UV scattered sunlight with SPICAM. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2006je002693] [Citation(s) in RCA: 25] [Impact Index Per Article: 1.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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37
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Bell JF, Savransky D, Wolff MJ. Chromaticity of the Martian sky as observed by the Mars Exploration Rover Pancam instruments. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2006je002687] [Citation(s) in RCA: 18] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- J. F. Bell
- Department of Astronomy; Cornell University; Ithaca New York USA
| | - D. Savransky
- Department of Astronomy; Cornell University; Ithaca New York USA
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38
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Newcombe DA, Schuerger AC, Benardini JN, Dickinson D, Tanner R, Venkateswaran K. Survival of spacecraft-associated microorganisms under simulated martian UV irradiation. Appl Environ Microbiol 2006; 71:8147-56. [PMID: 16332797 PMCID: PMC1317311 DOI: 10.1128/aem.71.12.8147-8156.2005] [Citation(s) in RCA: 86] [Impact Index Per Article: 4.8] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/20/2022] Open
Abstract
Spore-forming microbes recovered from spacecraft surfaces and assembly facilities were exposed to simulated Martian UV irradiation. The effects of UVA (315 to 400 nm), UVA+B (280 to 400 nm), and the full UV spectrum (200 to 400 nm) on the survival of microorganisms were studied at UV intensities expected to strike the surfaces of Mars. Microbial species isolated from the surfaces of several spacecraft, including Mars Odyssey, X-2000 (avionics), and the International Space Station, and their assembly facilities were identified using 16S rRNA gene sequencing. Forty-three Bacillus spore lines were screened, and 19 isolates showed resistance to UVC irradiation (200 to 280 nm) after exposure to 1,000 J m(-2) of UVC irradiation at 254 nm using a low-pressure mercury lamp. Spores of Bacillus species isolated from spacecraft-associated surfaces were more resistant than a standard dosimetric strain, Bacillus subtilis 168. In addition, the exposure time required for UVA+B irradiation to reduce the viable spore numbers by 90% was 35-fold longer than the exposure time required for the full UV spectrum to do this, confirming that UVC is the primary biocidal bandwidth. Among the Bacillus species tested, spores of a Bacillus pumilus strain showed the greatest resistance to all three UV bandwidths, as well as the total spectrum. The resistance to simulated Mars UV irradiation was strain specific; B. pumilus SAFR-032 exhibited greater resistance than all other strains tested. The isolation of organisms like B. pumilus SAFR-032 and the greater survival of this organism (sixfold) than of the standard dosimetric strains should be considered when the sanitation capabilities of UV irradiation are determined.
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Affiliation(s)
- David A Newcombe
- Biotechnology and Planetary Protection Group, Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
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39
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Johnson JR, Grundy WM, Lemmon MT, Bell JF, Johnson MJ, Deen RG, Arvidson RE, Farrand WH, Guinness EA, Hayes AG, Herkenhoff KE, Seelos F, Soderblom J, Squyres S. Spectrophotometric properties of materials observed by Pancam on the Mars Exploration Rovers: 1. Spirit. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2005je002494] [Citation(s) in RCA: 39] [Impact Index Per Article: 2.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
| | | | - Mark T. Lemmon
- Department of Atmospheric Sciences; Texas A&M University; College Station Texas USA
| | - James F. Bell
- Department of Astronomy; Cornell University; Ithaca New York USA
| | - Miles J. Johnson
- Department of Astronomy; Cornell University; Ithaca New York USA
| | - Robert G. Deen
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - Raymond E. Arvidson
- Department of Earth and Planetary Sciences; Washington University; St. Louis Missouri USA
| | | | - Edward A. Guinness
- Department of Earth and Planetary Sciences; Washington University; St. Louis Missouri USA
| | | | | | - Frank Seelos
- Department of Earth and Planetary Sciences; Washington University; St. Louis Missouri USA
| | - Jason Soderblom
- Department of Astronomy; Cornell University; Ithaca New York USA
| | - Steve Squyres
- Department of Astronomy; Cornell University; Ithaca New York USA
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40
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Golombek MP, Crumpler LS, Grant JA, Greeley R, Cabrol NA, Parker TJ, Rice JW, Ward JG, Arvidson RE, Moersch JE, Fergason RL, Christensen PR, Castaño A, Castaño R, Haldemann AFC, Li R, Bell JF, Squyres SW. Geology of the Gusev cratered plains from the Spirit rover transverse. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2005je002503] [Citation(s) in RCA: 97] [Impact Index Per Article: 5.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
Affiliation(s)
- M. P. Golombek
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - L. S. Crumpler
- New Mexico Museum of Natural History and Science; Albuquerque New Mexico USA
| | | | - R. Greeley
- Department of Geological Sciences; Arizona State University; Tempe Arizona USA
| | - N. A. Cabrol
- NASA Ames Research Center; Moffett Field California USA
| | - T. J. Parker
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - J. W. Rice
- Department of Geological Sciences; Arizona State University; Tempe Arizona USA
| | - J. G. Ward
- Department of Earth and Planetary Sciences; Washington University; St. Louis Missouri USA
| | - R. E. Arvidson
- Department of Earth and Planetary Sciences; Washington University; St. Louis Missouri USA
| | - J. E. Moersch
- Department of Geological Sciences; University of Tennessee; Knoxville Tennessee USA
| | - R. L. Fergason
- Department of Geological Sciences; Arizona State University; Tempe Arizona USA
| | - P. R. Christensen
- Department of Geological Sciences; Arizona State University; Tempe Arizona USA
| | - A. Castaño
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - R. Castaño
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - A. F. C. Haldemann
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - R. Li
- Department of Civil and Environmental Engineering and Geodetic Science; Ohio State University; Columbus Ohio USA
| | - J. F. Bell
- Department of Astronomy; Cornell University; Ithaca New York USA
| | - S. W. Squyres
- Department of Astronomy; Cornell University; Ithaca New York USA
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41
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Bell JF, Joseph J, Sohl-Dickstein JN, Arneson HM, Johnson MJ, Lemmon MT, Savransky D. In-flight calibration and performance of the Mars Exploration Rover Panoramic Camera (Pancam) instruments. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2005je002444] [Citation(s) in RCA: 96] [Impact Index Per Article: 5.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
Affiliation(s)
- J. F. Bell
- Department of Astronomy; Cornell University; Ithaca New York USA
| | - J. Joseph
- Department of Astronomy; Cornell University; Ithaca New York USA
| | | | - H. M. Arneson
- Department of Astronomy; Cornell University; Ithaca New York USA
| | - M. J. Johnson
- Department of Astronomy; Cornell University; Ithaca New York USA
| | - M. T. Lemmon
- Department of Atmospheric Sciences; Texas A&M University; College Station Texas USA
| | - D. Savransky
- Department of Astronomy; Cornell University; Ithaca New York USA
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42
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Montmessin F, Quémerais E, Bertaux JL, Korablev O, Rannou P, Lebonnois S. Stellar occultations at UV wavelengths by the SPICAM instrument: Retrieval and analysis of Martian haze profiles. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2005je002662] [Citation(s) in RCA: 77] [Impact Index Per Article: 4.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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43
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Kahre MA, Murphy JR, Haberle RM. Modeling the Martian dust cycle and surface dust reservoirs with the NASA Ames general circulation model. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2005je002588] [Citation(s) in RCA: 125] [Impact Index Per Article: 6.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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44
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Goetz W, Bertelsen P, Binau CS, Gunnlaugsson HP, Hviid SF, Kinch KM, Madsen DE, Madsen MB, Olsen M, Gellert R, Klingelhöfer G, Ming DW, Morris RV, Rieder R, Rodionov DS, de Souza PA, Schröder C, Squyres SW, Wdowiak T, Yen A. Indication of drier periods on Mars from the chemistry and mineralogy of atmospheric dust. Nature 2005; 436:62-5. [PMID: 16001062 DOI: 10.1038/nature03807] [Citation(s) in RCA: 110] [Impact Index Per Article: 5.8] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 11/23/2004] [Accepted: 04/29/2005] [Indexed: 11/08/2022]
Abstract
The ubiquitous atmospheric dust on Mars is well mixed by periodic global dust storms, and such dust carries information about the environment in which it once formed and hence about the history of water on Mars. The Mars Exploration Rovers have permanent magnets to collect atmospheric dust for investigation by instruments on the rovers. Here we report results from Mössbauer spectroscopy and X-ray fluorescence of dust particles captured from the martian atmosphere by the magnets. The dust on the magnets contains magnetite and olivine; this indicates a basaltic origin of the dust and shows that magnetite, not maghemite, is the mineral mainly responsible for the magnetic properties of the dust. Furthermore, the dust on the magnets contains some ferric oxides, probably including nanocrystalline phases, so some alteration or oxidation of the basaltic dust seems to have occurred. The presence of olivine indicates that liquid water did not play a dominant role in the processes that formed the atmospheric dust.
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Affiliation(s)
- Walter Goetz
- Max-Planck-Institut für Sonnensystemforschung, Katlenburg-Lindau, D-37191, Germany
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45
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Hartogh P, Medvedev AS, Kuroda T, Saito R, Villanueva G, Feofilov AG, Kutepov AA, Berger U. Description and climatology of a new general circulation model of the Martian atmosphere. ACTA ACUST UNITED AC 2005. [DOI: 10.1029/2005je002498] [Citation(s) in RCA: 57] [Impact Index Per Article: 3.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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46
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47
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Lemmon MT, Wolff MJ, Smith MD, Clancy RT, Banfield D, Landis GA, Ghosh A, Smith PH, Spanovich N, Whitney B, Whelley P, Greeley R, Thompson S, Bell JF, Squyres SW. Atmospheric imaging results from the Mars exploration rovers: Spirit and Opportunity. Science 2004; 306:1753-6. [PMID: 15576613 DOI: 10.1126/science.1104474] [Citation(s) in RCA: 188] [Impact Index Per Article: 9.4] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
A visible atmospheric optical depth of 0.9 was measured by the Spirit rover at Gusev crater and by the Opportunity rover at Meridiani Planum. Optical depth decreased by about 0.6 to 0.7% per sol through both 90-sol primary missions. The vertical distribution of atmospheric dust at Gusev crater was consistent with uniform mixing, with a measured scale height of 11.56 +/- 0.62 kilometers. The dust's cross section weighted mean radius was 1.47 +/- 0.21 micrometers (mm) at Gusev and 1.52 +/- 0.18 mm at Meridiani. Comparison of visible optical depths with 9-mm optical depths shows a visible-to-infrared optical depth ratio of 2.0 +/- 0.2 for comparison with previous monitoring of infrared optical depths.
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Affiliation(s)
- M T Lemmon
- Texas A&M University, College Station, TX 77843, USA.
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48
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Greeley R, Squyres SW, Arvidson RE, Bartlett P, Bell JF, Blaney D, Cabrol NA, Farmer J, Farrand B, Golombek MP, Gorevan SP, Grant JA, Haldemann AFC, Herkenhoff KE, Johnson J, Landis G, Madsen MB, McLennan SM, Moersch J, Rice JW, Richter L, Ruff S, Sullivan RJ, Thompson SD, Wang A, Weitz CM, Whelley P. Wind-related processes detected by the Spirit Rover at Gusev Crater, Mars. Science 2004; 305:810-3. [PMID: 15297660 DOI: 10.1126/science.1100108] [Citation(s) in RCA: 86] [Impact Index Per Article: 4.3] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Wind-abraded rocks, ripples, drifts, and other deposits of windblown sediments are seen at the Columbia Memorial Station where the Spirit rover landed. Orientations of these features suggest formative winds from the north-northwest, consistent with predictions from atmospheric models of afternoon winds in Gusev Crater. Cuttings from the rover Rock Abrasion Tool are asymmetrically distributed toward the south-southeast, suggesting active winds from the north-northwest at the time (midday) of the abrasion operations. Characteristics of some rocks, such as a two-toned appearance, suggest that they were possibly buried and exhumed on the order of 5 to 60 centimeters by wind deflation, depending on location.
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Affiliation(s)
- R Greeley
- Department of Geological Sciences, Arizona State University, Box 871404, Tempe, AZ 85287-1404, USA.
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49
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Squyres SW, Arvidson RE, Baumgartner ET, Bell JF, Christensen PR, Gorevan S, Herkenhoff KE, Klingelhöfer G, Madsen MB, Morris RV, Rieder R, Romero RA. Athena Mars rover science investigation. ACTA ACUST UNITED AC 2003. [DOI: 10.1029/2003je002121] [Citation(s) in RCA: 209] [Impact Index Per Article: 10.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- Steven W. Squyres
- Center for Radiophysics and Space Research; Cornell University; Ithaca New York USA
| | - Raymond E. Arvidson
- Department of Earth and Planetary Sciences; Washington University; St. Louis Missouri USA
| | | | - James F. Bell
- Department of Astronomy; Cornell University; Ithaca New York USA
| | | | | | | | - Göstar Klingelhöfer
- Institut für Anorganische Chemie und Analytische Chemie; Johannes Gutenberg University; Mainz Germany
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50
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Madsen MB, Bertelsen P, Goetz W, Binau CS, Olsen M, Folkmann F, Gunnlaugsson HP, Kinch KM, Knudsen JM, Merrison J, Nørnberg P, Squyres SW, Yen AS, Rademacher JD, Gorevan S, Myrick T, Bartlett P. Magnetic Properties Experiments on the Mars Exploration Rover mission. ACTA ACUST UNITED AC 2003. [DOI: 10.1029/2002je002029] [Citation(s) in RCA: 49] [Impact Index Per Article: 2.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- M. B. Madsen
- Center for Planetary Science, Niels Bohr Institute for Astronomy, Physics and Geophysics; University of Copenhagen; Copenhagen Denmark
| | - P. Bertelsen
- Center for Planetary Science, Niels Bohr Institute for Astronomy, Physics and Geophysics; University of Copenhagen; Copenhagen Denmark
| | - W. Goetz
- Center for Planetary Science, Niels Bohr Institute for Astronomy, Physics and Geophysics; University of Copenhagen; Copenhagen Denmark
| | - C. S. Binau
- Center for Planetary Science, Niels Bohr Institute for Astronomy, Physics and Geophysics; University of Copenhagen; Copenhagen Denmark
| | - M. Olsen
- Center for Planetary Science, Niels Bohr Institute for Astronomy, Physics and Geophysics; University of Copenhagen; Copenhagen Denmark
| | - F. Folkmann
- Department of Physics and Astronomy; University of Århus; Århus Denmark
| | | | - K. M. Kinch
- Department of Physics and Astronomy; University of Århus; Århus Denmark
| | - J. M. Knudsen
- Department of Physics and Astronomy; University of Århus; Århus Denmark
| | - J. Merrison
- Department of Physics and Astronomy; University of Århus; Århus Denmark
| | - P. Nørnberg
- Department of Earth Sciences; University of Århus; Århus Denmark
| | - S. W. Squyres
- Center for Radiophysics and Space Research, Astronomy Department; Cornell University; Ithaca USA
| | - A. S. Yen
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - J. D. Rademacher
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
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