Mars - Remote spectral identification of H2O frost and mineral hydrate

Details Mars - Remote spectral identification of H2O frost and mineral hydrate Mars - Remote spectral identification of H2O frost and mineral hydrate

Oct 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978pwpp.conf..100h&link_type=abstract

Planetary Water and Polar Processes, Proceedings of the Second Colloquium held 16-18 October, 1978 in Hanover, NH. Edited by Do

Computer Science

Hydrates, Mars (Planet), Planetary Composition, Polar Caps, Water, Absorption Spectra, Ice, Mars Sample Return Missions, Minerals, Planetology, Spectral Emission, Spectrometers, Spectrum Analysis

Scientific paper

A reflectance spectrum (0.62-2.6 microns) of Mars (integral disk) is obtained using a newly developed IR spectrometer at the 2.25 m telescope on Mauna Kea, Hawaii. Details of the instrument, observations, and data reduction are presented. Several distinct absorption features are evident that were apparently caused by H2O, but the positions and intensities of the features are quite unusual. In summary, the regolith is probably not as desiccated and dehydrated as the full disk reflectance spectrum and Viking soil analyses would suggest. The surface materials become desiccated and dehydrated as a result of solar UV effects and because of the relative adsorption and desorption rates during the strong diurnal cycling. There may be significant amounts of H2O at depth, and in the Solis Lacus region the H2O reservoir may extend to within a few centimeters of the surface. The Solis Lacus region may therefore be an important target for future Mars landing or sample return mission.

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