- Jeremie Lasue1,2,
- Nicolas Mangold3,
- Ernst Hauber4,
- Steve Clifford5,
- William Feldman6,
- Olivier Gasnault1,2,
- Cyril Grima7,
- Sylvestre Maurice1,2 &
- …
- Olivier Mousis1,2,8
1608Accesses
152Altmetric
21Mentions
Abstract
In this paper, we review current estimates of the global water inventory of Mars, potential loss mechanisms, the thermophysical characteristics of the different reservoirs that water may be currently stored in, and assess how the planet’s hydrosphere and cryosphere evolved with time. First, we summarize the water inventory quantified from geological analyses of surface features related to both liquid water erosion, and ice-related landscapes. They indicate that, throughout most of Martian geologic history (and possibly continuing through to the present day), water was present to substantial depths, with a total inventory ranging from several 100 to as much as 1000 m Global Equivalent Layer (GEL). We then review the most recent estimates of water content based on subsurface detection by orbital and landed instruments, including deep penetrating radars such as SHARAD and MARSIS. We show that the total amount of water measured so far is about 30 m GEL, although a far larger amount of water may be stored below the sounding depths of currently operational instruments. Finally, a global picture of the current state of the subsurface water reservoirs and their evolution is discussed.
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Acknowledgements
The authors thank the editor Mike Toplis, and 3 referees for careful comments on this manuscript. The authors also thank the staff of the International Space Science Institute (ISSI) in Bern, Switzerland for hospitality and assistance. Additional thanks to the HiRISE, MOC, MOLA, TES, THEMIS, SHARAD and MARSIS teams for providing excellent data to the scientific community. This work was partly supported by Los Alamos LDRD program. This is SC LPI contribution number 1704.
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Authors and Affiliations
UPS-OMP, IRAP, Université de Toulouse, Toulouse, France
Jeremie Lasue, Olivier Gasnault, Sylvestre Maurice & Olivier Mousis
CNRS, IRAP, 9 Av. colonel Roche, BP 44346, 31028, Toulouse cedex 4, France
Jeremie Lasue, Olivier Gasnault, Sylvestre Maurice & Olivier Mousis
Laboratoire Planétologie et Géodynamique de Nantes, CNRS and University of Nantes, 2, rue de la Houssinière, 44322, Nantes, France
Nicolas Mangold
DLR-Institut für Planetenforschung, Rutherfordstrasse 2, 12489, Berlin-Adlershof, Germany
Ernst Hauber
Lunar and Planetary Institute, 3600 Bay Area Boulevard, Houston, TX, 77058, USA
Steve Clifford
Planetary Science Institute, 1700 East Fort Lowell, Tucson, AZ, 85719, USA
William Feldman
Institute for Geophysics, Jackson School of Geosciences, University of Texas at Austin, Austin, TX, 78758, USA
Cyril Grima
Institut UTINAM, CNRS/INSU, UMR 6213, Observatoire des Sciences de l’Univers THETA, Université de Franche-Comté, Besançon, France
Olivier Mousis
- Jeremie Lasue
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- Nicolas Mangold
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- Ernst Hauber
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- Steve Clifford
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- William Feldman
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- Olivier Gasnault
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- Cyril Grima
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- Sylvestre Maurice
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- Olivier Mousis
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Correspondence toJeremie Lasue.
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Chapter in ISSI book “Quantifying the Martian geochemical reservoirs”.
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Lasue, J., Mangold, N., Hauber, E.et al. Quantitative Assessments of the Martian Hydrosphere.Space Sci Rev174, 155–212 (2013). https://doi.org/10.1007/s11214-012-9946-5
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