Spectroscopic identification of carbonate minerals in the martian dust.
Thermal infrared spectra of the martian surface indicate the presence of small concentrations (approximately 2 to 5 weight %) of carbonates, specifically dominated by magnesite (MgCO3). The carbonates are widely distributed in the martian dust, and there is no indication of a concentrated source. The presence of small concentrations of carbonate minerals in the surface dust and in martian meteorites can sequester several bars of atmospheric carbon dioxide and may have been an important sink for a thicker carbon dioxide atmosphere in the martian past.
Bandfield
Joshua L
JL
Department of Geological Sciences, Arizona State University, Tempe, AZ 85287-6305, USA. joshband@asu.edu
Glotch
Timothy D
TD
Christensen
Philip R
PR
D001272:Atmosphere; D001274:Atmospheric Pressure; D002245:Carbon Dioxide; D002254:Carbonates / Q000032:analysis*; D005118:Extraterrestrial Environment; D019015:Geologic Sediments; D008274:Magnesium / Q000032:analysis*; D018535:Mars; D019110:Meteoroids; D008903:Minerals / Q000032:analysis*; D010316:Particle Size; D017640:Silicates / Q000032:analysis; D013055:Spectrophotometry, Infrared; D014867:Water
D002254:Carbonates; D008903:Minerals; D017640:Silicates; D014867:Water; C005479:magnesium carbonate; D002245:Carbon Dioxide; D008274:Magnesium