Near infrared spectrophotometry of Mars at ESO.

Details Near infrared spectrophotometry of Mars at ESO. Near infrared spectrophotometry of Mars at ESO.

Jun 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989msngr..56...38e&link_type=abstract

The Messenger, vol. 56, p. 38-40

Mathematics

Logic

Mars: Infrared Spectrophotometry

Scientific paper

In spite of an extensive space exploration programme during the seventies, the planet Mars still raises several unresolved questions about the aeronomy of its atmosphere, the composition of its surface, and, more basically, the whole history of the planet. lnfrared spectroscopy has proven to be a major tool for these studies, as illustrated recently by the discovery of HDO at 3 ym and the measurement of the deuterium abundance (Owen et al., 1988). lnfrared spectroscopy between 1 and 5 ym is well adapted to the study of the martian atmosphere, as strong vibration bands of several atmospheric compounds (carbon dioxide, the major component, and minor constituents such as H20 and CO); it is also well suited, even with a low resolving power, for the study of mineralogic signatures of the martian surface (olivine, pyroxene, hydrated minerals, carbonates and other salts

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