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Greybush SJ, Kalnay E, Wilson RJ, Hoffman RN, Nehrkorn T, Leidner M, Eluszkiewicz J, Gillespie HE, Wespetal M, Zhao Y, Hoffman M, Dudas P, McConnochie T, Kleinböhl A, Kass D, McCleese D, Miyoshi T. The Ensemble Mars Atmosphere Reanalysis System (EMARS) Version 1.0. GEOSCIENCE DATA JOURNAL 2019; 6:137-150. [PMID: 31894192 PMCID: PMC6919928 DOI: 10.1002/gdj3.77] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 11/20/2018] [Revised: 07/02/2019] [Accepted: 07/25/2019] [Indexed: 05/15/2023]
Abstract
The Ensemble Mars Atmosphere Reanalysis System (EMARS) dataset version 1.0 contains hourly gridded atmospheric variables for the planet Mars, spanning Mars Year (MY) 24 through 33 (1999 through 2017). A reanalysis represents the best estimate of the state of the atmosphere by combining observations that are sparse in space and time with a dynamical model and weighting them by their uncertainties. EMARS uses the Local Ensemble Transform Kalman Filter (LETKF) for data assimilation with the GFDL/NASA Mars Global Climate Model (MGCM). Observations that are assimilated include the Thermal Emission Spectrometer (TES) and Mars Climate Sounder (MCS) temperature retrievals. The dataset includes gridded fields of temperature, wind, surface pressure, as well as dust, water ice, CO2 surface ice and other atmospheric quantities. Reanalyses are useful for both science and engineering studies, including investigations of transient eddies, the polar vortex, thermal tides and dust storms, and during spacecraft operations.
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Affiliation(s)
- Steven J. Greybush
- Department of Meteorology and Atmospheric ScienceThe Pennsylvania State UniversityUniversity ParkPAUSA
- Institute for CyberScienceThe Pennsylvania State UniversityUniversity ParkPAUSA
- Department of Atmospheric and Oceanic ScienceThe University of MarylandCollege ParkMDUSA
| | - Eugenia Kalnay
- Department of Atmospheric and Oceanic ScienceThe University of MarylandCollege ParkMDUSA
| | | | - Ross N. Hoffman
- Atmospheric and Environmental ResearchVerisk AnalyticsLexingtonMAUSA
| | - Thomas Nehrkorn
- Atmospheric and Environmental ResearchVerisk AnalyticsLexingtonMAUSA
| | - Mark Leidner
- Atmospheric and Environmental ResearchVerisk AnalyticsLexingtonMAUSA
| | | | - Hartzel E. Gillespie
- Department of Meteorology and Atmospheric ScienceThe Pennsylvania State UniversityUniversity ParkPAUSA
| | - Matthew Wespetal
- Department of Atmospheric and Oceanic ScienceThe University of MarylandCollege ParkMDUSA
| | - Yongjing Zhao
- Department of Atmospheric and Oceanic ScienceThe University of MarylandCollege ParkMDUSA
| | | | - Patrick Dudas
- Institute for CyberScienceThe Pennsylvania State UniversityUniversity ParkPAUSA
| | | | - Armin Kleinböhl
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - David Kass
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | | | - Takemasa Miyoshi
- Department of Atmospheric and Oceanic ScienceThe University of MarylandCollege ParkMDUSA
- RIKENKobeJapan
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Kereszturi A, Bradak B, Chatzitheodoridis E, Ujvari G. Indicators and Methods to Understand Past Environments from ExoMars Rover Drills. ORIGINS LIFE EVOL B 2016; 46:435-454. [PMID: 27029794 DOI: 10.1007/s11084-016-9492-3] [Citation(s) in RCA: 16] [Impact Index Per Article: 2.0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 07/28/2015] [Accepted: 01/15/2016] [Indexed: 11/26/2022]
Abstract
Great advances are expected during the analysis of drilled material acquired from 2 m depth by ExoMars rover, supported by the comparison to local context, and the joint use of different instruments. Textural information might be less detailed relatively to what is usually obtained at outcrops during classical geological field work on the Earth, partly because of the lack of optical imaging of the borehole wall and also because the collected samples are crushed. However sub-mm scale layering and some other sedimentary features might be identified in the borehole wall observations, or in the collected sample prior to crushing, and also at nearby outcrops. The candidate landing sites provide different targets and focus for research: Oxia Planum requires analysis of phyllosilicates and OH content, at Mawrth Vallis the layering of various phyllosilicates and the role of shallow-subsurface leaching should be emphasized. At Aram Dorsum the particle size and fluvial sedimentary features will be interesting. Hydrated perchlorates and sulphates are ideal targets possibly at every landing sites because of OH retention, especially if they are mixed with smectites, thus could point to even ancient wet periods. Extensive use of information from the infrared wall scanning will be complemented for geological context by orbital and rover imaging of nearby outcrops. Information from the context is especially useful to infer the possible action of past H2O. Separation of the ice and liquid water effects will be supported by cation abundance and sedimentary context. Shape of grains also helps here, and composition of transported grains points to the weathering potential of the environment in general. The work on Mars during the drilling and sample analysis will provide brand new experience and knowledge for future missions.
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Affiliation(s)
- A Kereszturi
- Research Centre for Astronomy and Earth Sciences, Budapest, Hungary.
| | - B Bradak
- Research Centre for Astronomy and Earth Sciences, Budapest, Hungary
- Department of Planetology, Kobe University, Kobe, Japan
| | | | - G Ujvari
- Research Centre for Astronomy and Earth Sciences, Budapest, Hungary
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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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Harri AM, Genzer M, Kemppinen O, Gomez-Elvira J, Haberle R, Polkko J, Savijärvi H, Rennó N, Rodriguez-Manfredi JA, Schmidt W, Richardson M, Siili T, Paton M, Torre-Juarez MDL, Mäkinen T, Newman C, Rafkin S, Mischna M, Merikallio S, Haukka H, Martin-Torres J, Komu M, Zorzano MP, Peinado V, Vazquez L, Urqui R. Mars Science Laboratory relative humidity observations: Initial results. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2014; 119:2132-2147. [PMID: 26213667 PMCID: PMC4508910 DOI: 10.1002/2013je004514] [Citation(s) in RCA: 6] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Received: 09/01/2013] [Accepted: 07/08/2014] [Indexed: 05/28/2023]
Abstract
UNLABELLED The Mars Science Laboratory (MSL) made a successful landing at Gale crater early August 2012. MSL has an environmental instrument package called the Rover Environmental Monitoring Station (REMS) as a part of its scientific payload. REMS comprises instrumentation for the observation of atmospheric pressure, temperature of the air, ground temperature, wind speed and direction, relative humidity (REMS-H), and UV measurements. We concentrate on describing the REMS-H measurement performance and initial observations during the first 100 MSL sols as well as constraining the REMS-H results by comparing them with earlier observations and modeling results. The REMS-H device is based on polymeric capacitive humidity sensors developed by Vaisala Inc., and it makes use of transducer electronics section placed in the vicinity of the three humidity sensor heads. The humidity device is mounted on the REMS boom providing ventilation with the ambient atmosphere through a filter protecting the device from airborne dust. The final relative humidity results appear to be convincing and are aligned with earlier indirect observations of the total atmospheric precipitable water content. The water mixing ratio in the atmospheric surface layer appears to vary between 30 and 75 ppm. When assuming uniform mixing, the precipitable water content of the atmosphere is ranging from a few to six precipitable micrometers. KEY POINTS Atmospheric water mixing ratio at Gale crater varies from 30 to 140 ppmMSL relative humidity observation provides good dataHighest detected relative humidity reading during first MSL 100 sols is RH75.
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Affiliation(s)
- A-M Harri
- Finnish Meteorological Institute Helsinki, Finland
| | - M Genzer
- Finnish Meteorological Institute Helsinki, Finland
| | - O Kemppinen
- Finnish Meteorological Institute Helsinki, Finland
| | | | - R Haberle
- NASA AMES Research Center San Francisco, California, USA
| | - J Polkko
- Finnish Meteorological Institute Helsinki, Finland
| | - H Savijärvi
- Finnish Meteorological Institute Helsinki, Finland
| | - N Rennó
- Department of Atmospheric, Oceanic and Space Sciences, University of Michigan Ann Arbor, Michigan, USA
| | | | - W Schmidt
- Finnish Meteorological Institute Helsinki, Finland
| | | | - T Siili
- Finnish Meteorological Institute Helsinki, Finland
| | - M Paton
- Finnish Meteorological Institute Helsinki, Finland
| | | | - T Mäkinen
- Finnish Meteorological Institute Helsinki, Finland
| | - C Newman
- Ashima Research Inc. Pasadena, California, USA
| | - S Rafkin
- Southwest Research Institute Boulder, Colorado, USA
| | - M Mischna
- NASA Jet Propulsion Laboratory Pasadena, California, USA
| | - S Merikallio
- Finnish Meteorological Institute Helsinki, Finland
| | - H Haukka
- Finnish Meteorological Institute Helsinki, Finland
| | | | - M Komu
- Finnish Meteorological Institute Helsinki, Finland
| | | | - V Peinado
- Centro de Astrobiologia Madrid, Spain
| | - L Vazquez
- Department of Applied Mathematics, Complutense University of Madrid Madrid, Spain
| | - R Urqui
- Centro de Astrobiologia Madrid, Spain
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Harri AM, Genzer M, Kemppinen O, Gomez-Elvira J, Haberle R, Polkko J, Savijärvi H, Rennó N, Rodriguez-Manfredi JA, Schmidt W, Richardson M, Siili T, Paton M, Torre-Juarez MDL, Mäkinen T, Newman C, Rafkin S, Mischna M, Merikallio S, Haukka H, Martin-Torres J, Komu M, Zorzano MP, Peinado V, Vazquez L, Urqui R. Mars Science Laboratory relative humidity observations: Initial results. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2014; 119:2132-2147. [PMID: 26213667 DOI: 10.1002/2013je004423] [Citation(s) in RCA: 7] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Received: 09/01/2013] [Accepted: 07/08/2014] [Indexed: 05/28/2023]
Abstract
UNLABELLED The Mars Science Laboratory (MSL) made a successful landing at Gale crater early August 2012. MSL has an environmental instrument package called the Rover Environmental Monitoring Station (REMS) as a part of its scientific payload. REMS comprises instrumentation for the observation of atmospheric pressure, temperature of the air, ground temperature, wind speed and direction, relative humidity (REMS-H), and UV measurements. We concentrate on describing the REMS-H measurement performance and initial observations during the first 100 MSL sols as well as constraining the REMS-H results by comparing them with earlier observations and modeling results. The REMS-H device is based on polymeric capacitive humidity sensors developed by Vaisala Inc., and it makes use of transducer electronics section placed in the vicinity of the three humidity sensor heads. The humidity device is mounted on the REMS boom providing ventilation with the ambient atmosphere through a filter protecting the device from airborne dust. The final relative humidity results appear to be convincing and are aligned with earlier indirect observations of the total atmospheric precipitable water content. The water mixing ratio in the atmospheric surface layer appears to vary between 30 and 75 ppm. When assuming uniform mixing, the precipitable water content of the atmosphere is ranging from a few to six precipitable micrometers. KEY POINTS Atmospheric water mixing ratio at Gale crater varies from 30 to 140 ppmMSL relative humidity observation provides good dataHighest detected relative humidity reading during first MSL 100 sols is RH75.
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Affiliation(s)
- A-M Harri
- Finnish Meteorological Institute Helsinki, Finland
| | - M Genzer
- Finnish Meteorological Institute Helsinki, Finland
| | - O Kemppinen
- Finnish Meteorological Institute Helsinki, Finland
| | | | - R Haberle
- NASA AMES Research Center San Francisco, California, USA
| | - J Polkko
- Finnish Meteorological Institute Helsinki, Finland
| | - H Savijärvi
- Finnish Meteorological Institute Helsinki, Finland
| | - N Rennó
- Department of Atmospheric, Oceanic and Space Sciences, University of Michigan Ann Arbor, Michigan, USA
| | | | - W Schmidt
- Finnish Meteorological Institute Helsinki, Finland
| | | | - T Siili
- Finnish Meteorological Institute Helsinki, Finland
| | - M Paton
- Finnish Meteorological Institute Helsinki, Finland
| | | | - T Mäkinen
- Finnish Meteorological Institute Helsinki, Finland
| | - C Newman
- Ashima Research Inc. Pasadena, California, USA
| | - S Rafkin
- Southwest Research Institute Boulder, Colorado, USA
| | - M Mischna
- NASA Jet Propulsion Laboratory Pasadena, California, USA
| | - S Merikallio
- Finnish Meteorological Institute Helsinki, Finland
| | - H Haukka
- Finnish Meteorological Institute Helsinki, Finland
| | | | - M Komu
- Finnish Meteorological Institute Helsinki, Finland
| | | | - V Peinado
- Centro de Astrobiologia Madrid, Spain
| | - L Vazquez
- Department of Applied Mathematics, Complutense University of Madrid Madrid, Spain
| | - R Urqui
- Centro de Astrobiologia Madrid, Spain
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Greybush SJ, Wilson RJ, Hoffman RN, Hoffman MJ, Miyoshi T, Ide K, McConnochie T, Kalnay E. Ensemble Kalman filter data assimilation of Thermal Emission Spectrometer temperature retrievals into a Mars GCM. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/2012je004097] [Citation(s) in RCA: 53] [Impact Index Per Article: 4.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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7
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Kadish SJ, Barlow NG, Head JW. Latitude dependence of Martian pedestal craters: Evidence for a sublimation-driven formation mechanism. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2008je003318] [Citation(s) in RCA: 62] [Impact Index Per Article: 4.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- Seth J. Kadish
- Department of Geological Sciences; Brown University; Providence Rhode Island USA
| | - Nadine G. Barlow
- Department of Physics and Astronomy; Northern Arizona University; Flagstaff Arizona USA
| | - James W. Head
- Department of Geological Sciences; Brown University; Providence Rhode Island USA
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8
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Kauhanen J, Siili T, Järvenoja S, Savijärvi H. The Mars limited area model and simulations of atmospheric circulations for the Phoenix landing area and season of operation. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je003011] [Citation(s) in RCA: 14] [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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9
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Richardson MI, Toigo AD, Newman CE. PlanetWRF: A general purpose, local to global numerical model for planetary atmospheric and climate dynamics. ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2006je002825] [Citation(s) in RCA: 186] [Impact Index Per Article: 10.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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10
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Montmessin F, Haberle RM, Forget F, Langevin Y, Clancy RT, Bibring JP. On the origin of perennial water ice at the south pole of Mars: A precession-controlled mechanism? ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2007je002902] [Citation(s) in RCA: 33] [Impact Index Per Article: 1.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- F. Montmessin
- Space Science Division; NASA Ames Research Center; Moffett Field USA
| | - R. M. Haberle
- Space Science Division; NASA Ames Research Center; Moffett Field USA
| | - F. Forget
- Laboratoire de Météorologie Dynamique; CNRS, IPSL, UPMC; Paris France
| | - Y. Langevin
- Institut d'Astrophysique Spatiale; Orsay Campus France
| | | | - J.-P. Bibring
- Institut d'Astrophysique Spatiale; Orsay Campus France
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11
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Levrard B, Forget F, Montmessin F, Laskar J. Recent formation and evolution of northern Martian polar layered deposits as inferred from a Global Climate Model. ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2006je002772] [Citation(s) in RCA: 95] [Impact Index Per Article: 5.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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12
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Shean DE, Head JW, Fastook JL, Marchant DR. Recent glaciation at high elevations on Arsia Mons, Mars: Implications for the formation and evolution of large tropical mountain glaciers. ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2006je002761] [Citation(s) in RCA: 68] [Impact Index Per Article: 4.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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13
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Keller JM, Boynton WV, Karunatillake S, Baker VR, Dohm JM, Evans LG, Finch MJ, Hahn BC, Hamara DK, Janes DM, Kerry KE, Newsom HE, Reedy RC, Sprague AL, Squyres SW, Starr RD, Taylor GJ, Williams RMS. Equatorial and midlatitude distribution of chlorine measured by Mars Odyssey GRS. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2006je002679] [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]
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14
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Hinson DP. Radio occultation measurements of transient eddies in the northern hemisphere of Mars. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2005je002612] [Citation(s) in RCA: 28] [Impact Index Per Article: 1.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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15
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Fedorova A, Korablev O, Bertaux JL, Rodin A, Kiselev A, Perrier S. Mars water vapor abundance from SPICAM IR spectrometer: Seasonal and geographic distributions. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2006je002695] [Citation(s) in RCA: 57] [Impact Index Per Article: 3.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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16
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Ivanov MA, Head JW. Alba Patera, Mars: Topography, structure, and evolution of a unique late Hesperian–early Amazonian shield volcano. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2005je002469] [Citation(s) in RCA: 30] [Impact Index Per Article: 1.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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17
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Montmessin F, Fouchet T, Forget F. Modeling the annual cycle of HDO in the Martian atmosphere. ACTA ACUST UNITED AC 2005. [DOI: 10.1029/2004je002357] [Citation(s) in RCA: 92] [Impact Index Per Article: 4.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- F. Montmessin
- NASA Ames Research Center; Moffett Field California USA
| | - T. Fouchet
- LESIA; Observatoire de Paris; Paris France
| | - F. Forget
- Laboratoire de Météorologie Dynamique; Institut Pierre Simon Laplace; Paris France
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18
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Richardson MI, Mischna MA. Long-term evolution of transient liquid water on Mars. ACTA ACUST UNITED AC 2005. [DOI: 10.1029/2004je002367] [Citation(s) in RCA: 69] [Impact Index Per Article: 3.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- Mark I. Richardson
- Division of Geological and Planetary Sciences; California Institute of Technology; Pasadena California USA
| | - Michael A. Mischna
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
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19
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Head JW, Neukum G, Jaumann R, Hiesinger H, Hauber E, Carr M, Masson P, Foing B, Hoffmann H, Kreslavsky M, Werner S, Milkovich S, van Gasselt S. Tropical to mid-latitude snow and ice accumulation, flow and glaciation on Mars. Nature 2005; 434:346-51. [PMID: 15772652 DOI: 10.1038/nature03359] [Citation(s) in RCA: 307] [Impact Index Per Article: 16.2] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 10/04/2004] [Accepted: 01/13/2005] [Indexed: 11/09/2022]
Abstract
Images from the Mars Express HRSC (High-Resolution Stereo Camera) of debris aprons at the base of massifs in eastern Hellas reveal numerous concentrically ridged lobate and pitted features and related evidence of extremely ice-rich glacier-like viscous flow and sublimation. Together with new evidence for recent ice-rich rock glaciers at the base of the Olympus Mons scarp superposed on larger Late Amazonian debris-covered piedmont glaciers, we interpret these deposits as evidence for geologically recent and recurring glacial activity in tropical and mid-latitude regions of Mars during periods of increased spin-axis obliquity when polar ice was mobilized and redeposited in microenvironments at lower latitudes. The data indicate that abundant residual ice probably remains in these deposits and that these records of geologically recent climate changes are accessible to future automated and human surface exploration.
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Affiliation(s)
- J W Head
- Department of Geological Sciences, Brown University, Providence, Rhode Island 02912, USA.
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Neukum G, Jaumann R, Hoffmann H, Hauber E, Head JW, Basilevsky AT, Ivanov BA, Werner SC, van Gasselt S, Murray JB, McCord T. Recent and episodic volcanic and glacial activity on Mars revealed by the High Resolution Stereo Camera. Nature 2005; 432:971-9. [PMID: 15616551 DOI: 10.1038/nature03231] [Citation(s) in RCA: 390] [Impact Index Per Article: 20.5] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/03/2004] [Accepted: 11/30/2004] [Indexed: 11/08/2022]
Abstract
The large-area coverage at a resolution of 10-20 metres per pixel in colour and three dimensions with the High Resolution Stereo Camera Experiment on the European Space Agency Mars Express Mission has made it possible to study the time-stratigraphic relationships of volcanic and glacial structures in unprecedented detail and give insight into the geological evolution of Mars. Here we show that calderas on five major volcanoes on Mars have undergone repeated activation and resurfacing during the last 20 per cent of martian history, with phases of activity as young as two million years, suggesting that the volcanoes are potentially still active today. Glacial deposits at the base of the Olympus Mons escarpment show evidence for repeated phases of activity as recently as about four million years ago. Morphological evidence is found that snow and ice deposition on the Olympus construct at elevations of more than 7,000 metres led to episodes of glacial activity at this height. Even now, water ice protected by an insulating layer of dust may be present at high altitudes on Olympus Mons.
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Affiliation(s)
- G Neukum
- Institut fuer Geologische Wissenschaften, Freie Universitaet Berlin, Malteserstrasse 74-100, Bldg D, 12249 Berlin, Germany.
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21
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Tokano T. Hydration state and abundance of zeolites on Mars and the water cycle. ACTA ACUST UNITED AC 2005. [DOI: 10.1029/2005je002410] [Citation(s) in RCA: 9] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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22
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Milkovich SM. North polar cap of Mars: Polar layered deposit characterization and identification of a fundamental climate signal. ACTA ACUST UNITED AC 2005. [DOI: 10.1029/2004je002349] [Citation(s) in RCA: 78] [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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23
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González-Galindo F. Extension of a Martian general circulation model to thermospheric altitudes: UV heating and photochemical models. ACTA ACUST UNITED AC 2005. [DOI: 10.1029/2004je002312] [Citation(s) in RCA: 55] [Impact Index Per Article: 2.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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24
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Shean DE. Origin and evolution of a cold-based tropical mountain glacier on Mars: The Pavonis Mons fan-shaped deposit. ACTA ACUST UNITED AC 2005. [DOI: 10.1029/2004je002360] [Citation(s) in RCA: 146] [Impact Index Per Article: 7.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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25
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Levrard B, Forget F, Montmessin F, Laskar J. Recent ice-rich deposits formed at high latitudes on Mars by sublimation of unstable equatorial ice during low obliquity. Nature 2004; 431:1072-5. [PMID: 15510141 DOI: 10.1038/nature03055] [Citation(s) in RCA: 162] [Impact Index Per Article: 8.1] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 04/08/2004] [Accepted: 09/17/2004] [Indexed: 11/09/2022]
Abstract
Observations from the gamma-ray spectrometer instrument suite on the Mars Odyssey spacecraft have been interpreted as indicating the presence of vast reservoirs of near-surface ice in high latitudes of both martian hemispheres. Ice concentrations are estimated to range from 70 per cent at 60 degrees latitude to 100 per cent near the poles, possibly overlain by a few centimetres of ice-free material in most places. This result is supported by morphological evidence of metres-thick layered deposits that are rich in water-ice and periglacial-like features found only at high latitudes. Diffusive exchange of water between the pore space of the regolith and the atmosphere has been proposed to explain this distribution, but such a degree of concentration is difficult to accommodate with such processes. Alternatively, there are suggestions that ice-rich deposits form by transport of ice from polar reservoirs and direct redeposition in high latitudes during periods of higher obliquity, but these results have been difficult to reproduce with other models. Here we propose instead that, during periods of low obliquity (less than 25 degrees), high-latitude ice deposits form in both hemispheres by direct deposition of ice, as a result of sublimation from an equatorial ice reservoir that formed earlier, during a prolonged high-obliquity excursion. Using the ice accumulation rates estimated from global climate model simulations we show that, over the past ten million years, large variations of Mars' obliquity have allowed the formation of such metres-thick, sedimentary layered deposits in high latitude and polar regions.
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Affiliation(s)
- Benjamin Levrard
- Astronomie et Systèmes Dynamiques, IMC-CNRS UMR8028, 77 Avenue Denfert-Rochereau, 75014 Paris, France.
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Montmessin F. Origin and role of water ice clouds in the Martian water cycle as inferred from a general circulation model. ACTA ACUST UNITED AC 2004. [DOI: 10.1029/2004je002284] [Citation(s) in RCA: 236] [Impact Index Per Article: 11.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Hinson DP. Temperature inversions, thermal tides, and water ice clouds in the Martian tropics. ACTA ACUST UNITED AC 2004. [DOI: 10.1029/2003je002129] [Citation(s) in RCA: 95] [Impact Index Per Article: 4.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Golombek MP, Grant JA, Parker TJ, Kass DM, Crisp JA, Squyres SW, Haldemann AFC, Adler M, Lee WJ, Bridges NT, Arvidson RE, Carr MH, Kirk RL, Knocke PC, Roncoli RB, Weitz CM, Schofield JT, Zurek RW, Christensen PR, Fergason RL, Anderson FS, Rice JW. Selection of the Mars Exploration Rover landing sites. ACTA ACUST UNITED AC 2003. [DOI: 10.1029/2003je002074] [Citation(s) in RCA: 126] [Impact Index Per Article: 6.0] [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
| | - T. J. Parker
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - D. M. Kass
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - J. A. Crisp
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - S. W. Squyres
- Department of Astronomy; Cornell University; Ithaca New York USA
| | - A. F. C. Haldemann
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - M. Adler
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - W. J. Lee
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - N. T. Bridges
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - R. E. Arvidson
- Department of Earth and Space Sciences; Washington University; St. Louis Missouri USA
| | - M. H. Carr
- U.S. Geological Survey; Menlo Park California USA
| | - R. L. Kirk
- U.S. Geological Survey; Flagstaff Arizona USA
| | - P. C. Knocke
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - R. B. Roncoli
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | | | - J. T. Schofield
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - R. W. Zurek
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - P. R. Christensen
- Department of Geological Sciences; Arizona State University; Tempe Arizona USA
| | - R. L. Fergason
- Department of Geological Sciences; Arizona State University; Tempe Arizona USA
| | - F. S. Anderson
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - J. W. Rice
- Department of Geological Sciences; Arizona State University; Tempe Arizona USA
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Head JW, Mustard JF, Kreslavsky MA, Milliken RE, Marchant DR. Recent ice ages on Mars. Nature 2003; 426:797-802. [PMID: 14685228 DOI: 10.1038/nature02114] [Citation(s) in RCA: 606] [Impact Index Per Article: 28.9] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 05/16/2003] [Accepted: 10/08/2003] [Indexed: 11/09/2022]
Abstract
A key pacemaker of ice ages on the Earth is climatic forcing due to variations in planetary orbital parameters. Recent Mars exploration has revealed dusty, water-ice-rich mantling deposits that are layered, metres thick and latitude dependent, occurring in both hemispheres from mid-latitudes to the poles. Here we show evidence that these deposits formed during a geologically recent ice age that occurred from about 2.1 to 0.4 Myr ago. The deposits were emplaced symmetrically down to latitudes of approximately 30 degrees--equivalent to Saudi Arabia and the southern United States on the Earth--in response to the changing stability of water ice and dust during variations in obliquity (the angle between Mars' pole of rotation and the ecliptic plane) reaching 30-35 degrees. Mars is at present in an 'interglacial' period, and the ice-rich deposits are undergoing reworking, degradation and retreat in response to the current instability of near-surface ice. Unlike the Earth, martian ice ages are characterized by warmer polar climates and enhanced equatorward transport of atmospheric water and dust to produce widespread smooth deposits down to mid-latitudes.
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Affiliation(s)
- James W Head
- Department of Geological Sciences, Brown University, Providence, Rhode Island 02912, USA.
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Toigo AD, Richardson MI. Meteorology of proposed Mars Exploration Rover landing sites. ACTA ACUST UNITED AC 2003. [DOI: 10.1029/2003je002064] [Citation(s) in RCA: 37] [Impact Index Per Article: 1.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- Anthony D. Toigo
- Center for Radiophysics and Space Research; Cornell University; Ithaca New York USA
| | - Mark I. Richardson
- Division of Geological and Planetary Sciences; California Institute of Technology; Pasadena California USA
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Liu J. An assessment of the global, seasonal, and interannual spacecraft record of Martian climate in the thermal infrared. ACTA ACUST UNITED AC 2003. [DOI: 10.1029/2002je001921] [Citation(s) in RCA: 87] [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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Mischna MA. On the orbital forcing of Martian water and CO2cycles: A general circulation model study with simplified volatile schemes. ACTA ACUST UNITED AC 2003. [DOI: 10.1029/2003je002051] [Citation(s) in RCA: 184] [Impact Index Per Article: 8.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Richardson MI, Wilson RJ. A topographically forced asymmetry in the martian circulation and climate. Nature 2002; 416:298-301. [PMID: 11907570 DOI: 10.1038/416298a] [Citation(s) in RCA: 111] [Impact Index Per Article: 5.0] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/08/2022]
Abstract
Large seasonal and hemispheric asymmetries in the martian climate system are generally ascribed to variations in solar heating associated with orbital eccentricity. As the orbital elements slowly change (over a period of >104 years), characteristics of the climate such as dustiness and the vigour of atmospheric circulation are thought to vary, as should asymmetries in the climate (for example, the deposition of water ice at the northern versus the southern pole). Such orbitally driven climate change might be responsible for the observed layering in Mars' polar deposits by modulating deposition of dust and water ice. Most current theories assume that climate asymmetries completely reverse as the angular distance between equinox and perihelion changes by 180 degrees. Here we describe a major climate mechanism that will not precess in this way. We show that Mars' global north-south elevation difference forces a dominant southern summer Hadley circulation that is independent of perihelion timing. The Hadley circulation, a tropical overturning cell responsible for trade winds, largely controls interhemispheric transport of water and the bulk dustiness of the atmosphere. The topography therefore imprints a strong handedness on climate, with water ice and the active formation of polar layered deposits more likely in the north.
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Affiliation(s)
- Mark I Richardson
- Division of Geological and Planetary Sciences, California Institute of Technology, MC 150-21, Pasadena, California 91125, USA.
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Richardson MI. Water ice clouds in the Martian atmosphere: General circulation model experiments with a simple cloud scheme. ACTA ACUST UNITED AC 2002. [DOI: 10.1029/2001je001804] [Citation(s) in RCA: 67] [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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