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A coordinated spectral, mineralogical, and compositional study of ordinary chondrites |
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| Authors: | Tasha L Dunn Timothy J McCoy Harry Y McSween Jr |
| Institution: | a Department of Earth and Planetary Sciences, Planetary Geosciences Institute, University of Tennessee, Knoxville, TN 37902, USA b Department of Mineral Sciences, National Museum of Natural History, Smithsonian Institution, Washington, DC 20013-7012, USA c Department of Astronomy, University of Maryland, College Park, MD 20742-2421, USA d Department of Geography-Geology, Illinois State University, Normal, IL 61761, USA |
| Abstract: | Mineral compositions and abundances derived from visible/near-infrared (VIS/NIR or VNIR) spectra are used to classify asteroids, identify meteorite parent bodies, and understand the structure of the asteroid belt. Using a suite of 48 equilibrated (types 4-6) ordinary (H, L, and LL) chondrites containing orthopyroxene, clinopyroxene, and olivine, new relationships between spectra and mineralogy have been established. Contrary to previous suggestions, no meaningful correlation is observed between band parameters and cpx/(opx + cpx) ratios. We derive new calibrations for determining mineral abundances (ol/(ol + px)) and mafic silicate compositions (Fa in olivine, Fs in pyroxene) from VIS/NIR spectra. These calibrations confirm that band area ratio (BAR) is controlled by mineral abundances, while Band I center is controlled by mafic silicate compositions. Spectrally-derived mineralogical parameters correctly classify H, L and LL chondrites in ∼80% of cases, suggesting that these are robust relationships that can be applied to S(IV) asteroids with ordinary chondrites mineralogies. Comparison of asteroids and meteorites using these new mineralogical parameters has the advantage that H, L and LL chemical groups were originally defined on the basis of mafic silicate compositions. |
| Keywords: | Asteroids Spectroscopy Meteorites |
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