Vesta and HED Meteorites: Determining Minerals and their Abundances with Mid-IR Spectral Deconvolution I

Details Vesta and HED Meteorites: Determining Minerals and their Abundances with Mid-IR Spectral Deconvolution I Vesta and HED Meteorites: Determining Minerals and their Abundances with Mid-IR Spectral Deconvolution I

Oct 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007dps....39.3308h&link_type=abstract

American Astronomical Society, DPS meeting #39, #33.08; Bulletin of the American Astronomical Society, Vol. 39, p.477

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We identify the known mineral compositions and abundances of laboratory samples of Howardite, Eucrite and Diogenite (HED) meteorites (Salisbury et al. 1991, Icarus 9, 280-297) using an established spectral deconvolution algorithm (Ramsey, 1996 Ph.D. Dissertation, ASU; Ramsey and Christiansen 1998, JGR 103, 577-596) for mid-infrared spectral libraries of mineral separates of varying grain sizes. Most notably, the spectral deconvolution algorithm fit the known plagioclase and pyroxene compositions for all of the HED meteorite spectra determined by laboratory analysis. Our results for the HED samples, give us a high degree of confidence that our results are valid and that the spectral deconvolution algorithm is viable. Mineral compositions and abundances are also determined using the same technique for one possible HED parent body, Vesta, using mid-infrared spectra that were obtained from ground-based telescopes (Sprague et al. 1993, A.S.P. 41 Lim et al. 2005, Icarus 173, 385-408) and the Infrared Space Observatory (ISO) (Dotto et al. 2000, A&A 358, 1133-1141). Mid-infrared spectra of Vesta come from different areas on its surface. The ISO Vesta spectral deconvolution is suggestive of triolite, olivine, augite, chromite, wollastonite, and sodalite at one location. Modeling of other locations is underway. We also were successful in modeling spectra from locations on the Moon where no Apollo samples are available and for several locations on Mercury's surface using the same techniques (see lunar and mercurian abstracts this meeting). These results demonstrate promise for the spectral deconvolution method to correctly make mineral identifications on remotely observed objects, in particular main-belt asteroids, the Moon, and Mercury. This work was funded by NSF AST0406796.

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