Measurements of Water Ice from Martian Orbit and on the Surface

Details Measurements of Water Ice from Martian Orbit and on the Surface Measurements of Water Ice from Martian Orbit and on the Surface

Jul 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000came.work..227m&link_type=abstract

Concepts and Approaches for Mars Exploration, p. 227

Computer Science

Mars Surface, Water, Ice, Mars (Planet), Mars Missions, Neutrons, Detection, Mars Surveyor 2001 Mission, Mission Planning, Neutron Spectrometers, Gamma Ray Spectrometers

Scientific paper

Cosmic rays are known to produce large number of high-energy neutrons at the Martian surface. These neutrons produce gamma-ray lines from the nucleus either via inelastic scattering (I-type lines), in which they keep their original high energy, or via capturing reactions (C-type lines), in which they are slowed down to epithermal or thermal energies. These lines together with the lines produced by natural decay of K, Th, and U (N-type lines) will be measured by the Gamma-Ray Spectrometer (GRS) with high purity Ge detector. The mapping of these lines will allow the investigators to determine the distribution of the principal minerals globally over the Martian surface, which is one of the primarily goals of the Mars Surveyor Orbiter 2001 mission. The main scientific objectives of Russian High Energy Neutron Detector (HEND) are consistent with this goal. HEND, as a part of GRS facility, will provide the map of high-energy neutron albedo, which will allow (together with the complementary map of low energy neutron albedo from the Neutron Spectrometer (NS)) to distinguish I-type, C-type, and N-type lines among the forest of lines from the GRS.

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