Spectroscopy of B-Type Asteroids: Subgroups and Meteorite Analogs

Details Spectroscopy of B-Type Asteroids: Subgroups and Meteorite Analogs Spectroscopy of B-Type Asteroids: Subgroups and Meteorite Analogs

Sep 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009dps....41.3208c&link_type=abstract

American Astronomical Society, DPS meeting #41, #32.08

Astronomy and Astrophysics

Astronomy

Scientific paper

B-type asteroids have a negative slope from 0.5 to 1.1 microns and beyond. What causes this? Visible to near-infrared reflectance spectra (0.4 to 2.5 microns) are assembled for 22 B-type asteroids. The spectra fall naturally into three groups: 1) those with negative (blue) spectral shapes like 2 Pallas; 2) those with concave curve shapes like 24 Themis; and 3) everything else. The asteroid spectra are compared with mineral and meteorite spectra from the RELAB library of 15,000 samples, in a least-squares search for particulate analogs, constrained by spectral brightness. The Pallas group meteorite matches show a trend of "dry” analogs, such as CV, CO, and CK-meteorites. The Themis group meteorite matches show a trend of "wet” or "previously wet” analogs, such as CI, CM, CR, and CI- or CM-Unusual meteorites. Allowing for reasonable uncertainties in the spectral matches, we find no need to invoke mineralogies that do not exist in the meteorite collection to explain B-type spectra. Our Themis group results are as expected, and are consistent with previous work, but our Pallas group results are new, surprising, problematic, and in conflict with previous work.

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