Thermal emission spectra of Mars (5.4-10.5 microns) - Evidence for sulfates, carbonates, and hydrates

Details Thermal emission spectra of Mars (5.4-10.5 microns) - Evidence for sulfates, carbonates, and hydrates Thermal emission spectra of Mars (5.4-10.5 microns) - Evidence for sulfates, carbonates, and hydrates

Aug 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990jgr....9514595p&link_type=abstract

(American Geophysical Union and Geological Society of America, International Conference on Mars, 4th, Tucson, AZ, Jan. 10-13, 19

Mathematics

Logic

116

Carbonates, Emission Spectra, Hydrates, Mars Surface, Planetary Radiation, Sulfates, Thermal Emission, Atmospheric Composition, Carbon Dioxide Concentration, Mars Atmosphere, Surface Temperature

Scientific paper

Spectra of the Martian thermal emission in the 5.4-10.5 micron region are reported. Emission features at 7.8 and 9.7 microns are attributed to surface silicates, and an emission feature at 6.1 micron is attributed to a molecular water component of the surface material. An absorption band at 8.7 micron and a possible one at 9.8 microns is attributed to sulfate or bisulfate anions probably located at a distorted crystalline site, and an absorption band at 6.7 microns is attributed to carbonate or bicarbonate anions located in a distorted crystalline site. Spectral simulations indicate that the sulfate- and carbonate-bearing minerals are contained in the same particles of airborne dust as the dominant silicate minerals, that the dust optical depth is about 0.6 at a reference wavelength of 0.3 micron over the area of the observed spots, and that sulfates and carbonates constitute 10-15 percent and 1-3 percent by volume of the airborne dust, respectively.

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