A composite mineralogical map of Ganges Chasma and surroundings, Valles Marineris, Mars

Cull-Hearth, Selby; Clark, M. Caroline

doi:10.1016/j.pss.2017.03.011

Cited by 5 publications

(1 citation statement)

References 37 publications

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“…The presence of water ice inside Valles Marineris has been suggested by several studies (Gourronc et al., 2014; Jakosky et al., 2005; Schorghofer & Aharonson, 2005; Schorghofer & Forget, 2012; Vincendon et al., 2010), while others proposed strong opposing arguments based on its close proximity to equator (Cull‐Hearth & Clark, 2017; le Deit et al., 2010; Roach et al., 2010; Weitz et al., 2015). Derived values of WEH for the first and second sub‐regions of LWRR‐1 present rather strong arguments in favor of the presence of water ice because it seems unlikely that any other form of water may have such a large mass fraction in the shallow subsurface, except ice.…”

Section: Several Examples Of Detected Local Water‐rich Regionsmentioning

confidence: 97%

High Resolution Map of Water in the Martian Regolith Observed by FREND Neutron Telescope Onboard ExoMars TGO

et al. 2022

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Introduction Measuring Water Content in Marstian Regolith Through Neutron FluxWater in the upper meter of Martian regolith is found practically everywhere on the planet using remote neutron and gamma ray sensing methods. It is most abundant in the polar regions above 60° latitude, where its content measured as Water Equivalent Hydrogen is higher than 40 wt% (WEH is a measure of water in weight percent (wt%) that the subsurface material contains in case all hydrogen is attributed to water molecules, H 2 O). Such large amounts of WEH most probably mean presence of subsurface water ice. On the other hand, moderate latitudes between 40° north and south only show several wt% WEH (Boynton et al., 2002;Feldman et al., 2002;Mitrofanov et al., 2002). In this case hydrogen is thought to be attributed to either adsorbed water or water chemically bound in hydrated minerals. Some studies (e.g., Byrne et al., 2009) suggested that water ice might be present in the subsurface even in some equatorial areas with favorable conditions. In any case, water content mapping is of scientific interest, providing insights to hydrologic history of Mars. Moreover, its present conditions are an invaluable resource for planning future robotic and human exploration.The mapping of water mentioned above was carried out through neutron and gamma ray sensing instruments. This technique is widely known and was performed on Martian orbit by three instruments in the past (Boynton et al., 2002;Feldman et al., 2002;Mitrofanov et al., 2002). It was described in details, for example, in (Drake et al., 1988;Masarik & Reedy, 1996). Galactic Cosmic Rays (GCRs) bombard the surface of a celestial body with no or thin atmosphere, penetrating its regolith to a depth of about 2 m. As a result, particles of GCRs collide with the soil constituting nuclei and produce fast neutrons, some of which leak back toward the surface and can be detected by an orbital or lander instrument. As neutrons leak, they are moderated (loose energy

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