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The Moon: Determining Minerals and their Abundances with Mid-IR Spectral Deconvolution II
Uppsala University.
2007 (English)Conference paper (Other (popular scientific, debate etc.))
Abstract [en]

We determine the mineral compositions and abundances at three locations on the lunar surface 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. Spectral measurements of the lunar surface were obtained at the Infrared Telescope Facility (IRTF) on Mauna Kea, HI with Boston University's Mid-Infrared Spectrometer and Imager (MIRSI). Our chosen locations, Aristarchus, Grimaldi and Mersenius C, have been previously observed in the VIS near-IR from ground-based telescopes and spacecraft (Zisk et al. 1977, The Moon 17, 59-99; Hawke et al. 1993, GRL 20, 419-422; McEwen et al. 1994, Science 266, 1858-1862; Peterson et al. 1995, 22, 3055-3058; Warell et al. 2006, Icarus 180, 281-291), however there are no sample returns for analysis. Surface mineral deconvolutions of the Grimaldi Basin infill are suggestive of anorthosite, labradorite, orthopyroxene, olivine, garnet and phosphate. Peterson et al. (1995) indicated the infill of Grimaldi Basin has a noritic anorthosite or anorthositic norite composition. Our spectral deconvolution supports these results. Modeling of other lunar locations is underway. We have also successfully modeled laboratory spectra of HED meteorites, Vesta, and Mercury (see meteorites and mercurian abstracts this meeting). These results demonstrate the spectral deconvolution method to be robust for making mineral identifications on remotely observed objects, in particular main-belt asteroids, the Moon, and Mercury. This work was funded by NSF AST406796.

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URN: urn:nbn:se:uu:diva-13802OAI: oai:DiVA.org:uu-13802DiVA: diva2:41572
Available from: 2008-01-25 Created: 2008-01-25

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Warell, Johan
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