%0 Journal Article %1 Feldman2004 %A Feldman, W. C. %A Mellon, M. T. %A Maurice, S. %A Prettyman, T. H. %A Carey, J. W. %A Vaniman, D. T. %A Bish, D. L. %A Fialips, C. I. %A Chipera, S. J. %A Kargel, J. S. %A Elphic, R. C. %A Funsten, H. O. %A Lawrence, D. J. %A Tokar, R. L. %D 2004 %J Geophysical Research Letters %K BEHAVIOR; GROUND ICE; MARTIAN MINERALS; MODEL STABILITY; SURFACE; WATER; %N 16 %P L16702 %T Hydrated states of MgSO4 at equatorial latitudes on Mars %V 31 %X The stability of water ice, epsomite, and hexahydrite to loss of H2O molecules to the atmosphere at equatorial latitudes of Mars was studied to determine their potential contributions to the measured abundance of water-equivalent hydrogen (WEH). Calculation of the relative humidity based on estimates of yearly averages of water-vapor pressures and temperatures at the Martian surface was used for this purpose. Water ice was found to be sufficiently unstable everywhere within 45degrees of the equator that if the observed WEH is due to water ice, it requires a low-permeability cover layer near the surface to isolate the water ice below from the atmosphere above. In contrast, epsomite or hexahydrite may be stable in many near-equatorial locations where significant amounts of WEH are observed.

@article{Feldman2004, abstract = {The stability of water ice, epsomite, and hexahydrite to loss of H2O molecules to the atmosphere at equatorial latitudes of Mars was studied to determine their potential contributions to the measured abundance of water-equivalent hydrogen (WEH). Calculation of the relative humidity based on estimates of yearly averages of water-vapor pressures and temperatures at the Martian surface was used for this purpose. Water ice was found to be sufficiently unstable everywhere within 45degrees of the equator that if the observed WEH is due to water ice, it requires a low-permeability cover layer near the surface to isolate the water ice below from the atmosphere above. In contrast, epsomite or hexahydrite may be stable in many near-equatorial locations where significant amounts of WEH are observed.}, added-at = {2009-11-03T20:21:25.000+0100}, author = {Feldman, W. C. and Mellon, M. T. and Maurice, S. and Prettyman, T. H. and Carey, J. W. and Vaniman, D. T. and Bish, D. L. and Fialips, C. I. and Chipera, S. J. and Kargel, J. S. and Elphic, R. C. and Funsten, H. O. and Lawrence, D. J. and Tokar, R. L.}, biburl = {https://www.bibsonomy.org/bibtex/27b0c4f90ea8ed7f65737f78ffa898fde/svance}, citedreferences = {BASILEVSKY AT, 2003, SOLAR SYST RES+, V37, P387 ; BISH DL, 2003, 6 INT C MARS JET PRO ; BISH DL, 2003, Icarus, V164, P96 ; CHOU IM, 2003, Astrobiology, V3, P619 ; CHRISTENSEN PR, 2001, J GEOPHYS RES-PLANET, V106, P23823 ; CLARK BC, 1978, Icarus, V34, P645 ; CLIFFORD SM, 1983, J GEOPHYS RES, V88, P2456 ; CLIFFORD SM, 1993, J GEOPHYS RES-PLANET, V98, P10973 ; CLIFFORD SM, 1998, LUNAR PLANET SCI, V29 ; FANALE FP, 1986, Icarus, V67, P1 ; FARMER CB, 1979, J GEOPHYS RES, V84, P2881 ; FELDMAN WC, 2004, IN PRESS J GEOPHYS R ; FIALIPS CI, 2004, LUNAR PLANET SCI, V35 ; GOODING JL, 1992, PHYSICAL CHEM WEATHE, P626 ; MELLON MT, 1993, J GEOPHYS RES-PLANET, V98, P3345 ; MELLON MT, 1995, J GEOPHYS RES-PLANET, V100, P11781 ; MELLON MT, 2002, LUNAR PLANET SCI, V33 ; MELLON MT, 2004, Icarus, V169, P324 ; MOHLMANN DTF, 2004, Icarus, V168, P318 ; PAIGE DA, 1994, J GEOPHYS RES, V99, P25992 ; PRETTYMAN TH, 2004, J GEOPHYS RES, V109 ; SMITH DE, 1999, Science, V284, P1495 ; TOKANO T, 2003, Icarus, V164, P50 ; VAINMAN DT, 2004, LUNAR PLANET SCI, V35, P1690 ; WANKE H, 2001, SPACE SCI REV, V96, P317 ; ZOLOTOV MY, 1989, LUNAR PLANET SCI, V20, P1257}, interhash = {b165f0b01d4174ee7be69f769c7057f9}, intrahash = {7b0c4f90ea8ed7f65737f78ffa898fde}, journal = {Geophysical Research Letters}, keywords = {BEHAVIOR; GROUND ICE; MARTIAN MINERALS; MODEL STABILITY; SURFACE; WATER;}, number = 16, owner = {svance}, pages = {L16702}, timestamp = {2009-11-03T20:21:47.000+0100}, title = {Hydrated states of MgSO4 at equatorial latitudes on Mars}, volume = 31, year = 2004 }