Abstract
ABSTRACT The Mars Odyssey Neutron Spectrometer (MONS) is described and its capabilities to detect and quantify deposits of H and CO 2 ice within about 1 m of the surface are presented. After two Martian years in mapping orbit about Mars, two distinct domains of hydrogen deposits have been delimited. High-latitude domains in both hemispheres contain large, generally buried deposits of hydrogen and a near-equatorial domain contains more modest, yet significant, deposits. All observations are specified in units of water-equivalent hydrogen (WEH) and are compared with other observations of near-surface deposits of H 2 O and OH. They are also discussed in terms of theoretical models of volatile exchange between different water reservoirs through the atmosphere or through a system of aquifers. The CO 2 ice cover of the residual cap near the South Pole is modeled and found not to be a significant part of the CO 2 inventory of Mars.
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