The Silicate Chemistry of the A-type Asteroids

Details The Silicate Chemistry of the A-type Asteroids The Silicate Chemistry of the A-type Asteroids

Jul 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997dps....29.0708w&link_type=abstract

American Astronomical Society, DPS meeting #29, #07.08; Bulletin of the American Astronomical Society, Vol. 29, p.973

Astronomy and Astrophysics

Astronomy

Scientific paper

Previously obtained high quality near-infrared spectra of asteroids revealed that a class of objects, the A-types, have spectra which are quite similar to the mineral olivine. We compared the spectra of asteroids 446 Aeternitas, 289 Nenettta, 246 Asporina, and 863 Benkoela with a series of powdered laboratory olivines of varying Fe content. We conclude that the 1.05 micron olivine feature in all four asteroids is identical to the same feature in very Fe-poor laboratory olivines. The presence of very low Fe olivine indicates that the objects' origin lies in a reduced parent body, unlike most common meteorite types. The only meteorite type with a monomineralic olivine silicate fraction and this unusual Fe-poor olivine chemistry is the main group of pallasites. Thus it seems likely that the well-known A-type asteroids are the parent bodies of the main group of pallasite meteorites, and are not metal-free olivine assemblages.

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