First direct detection of clay minerals on Mars

Details First direct detection of clay minerals on Mars First direct detection of clay minerals on Mars

Apr 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985pggp.rept..391s&link_type=abstract

In NASA, Washington Repts. of Planetary Geol. and Geophys. Program, 1984 p 391-392 (SEE N85-23474 13-91)

Astronomy and Astrophysics

Astronomy

Absorption Spectra, Clays, Mars Surface, Minerals, Planetary Composition, Astronomical Spectroscopy, Infrared Spectra, Magnesium, Regolith

Scientific paper

Magnesian clays or clay-type minerals were conclusively detected in the martian regolith. Near-IR spectral observations of Mars using the Mauna Kea 2.2-m telescope show weak but definite absorption bands near microns. The absorption band positions and widths match those produced by combined OH stretch and Mg-OH lattice modes and are diagnostic of minerals with structural OH such as clays and amphiboles. Likely candidate minerals include serpentine, talc, hectorite, and sponite. There is no spectral evidence for aluminous hydroxylated minerals. No distinct band occurs at 2.55 microns, as would be expected if carbonates were responsible for the 2.35 micron absorption. High-albedo regions such as Elysium and Utopia have the strongest bands near 2.35 microns, as would be expected for heavily weathered soils. Low-albedo regions such as Iapygia show weaker but distinct bands, consistent with moderate coatings, streaks, and splotches of bright weathered material. In all areas observed, the 2.35-micron absorption is at least three times weaker than would be expected if well-crystallized clay minerals made up the bulk of bright soils on Mars.

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