Other
Scientific paper
Feb 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004jgre..10902001c&link_type=abstract
Journal of Geophysical Research, Volume 109, Issue E2, CiteID E02001
Other
28
Planetology: Solar System Objects: Asteroids And Meteoroids, Planetology: Solar System Objects: Meteorites And Tektites, Planetology: Solid Surface Planets: Composition, Planetology: Comets And Small Bodies: Radiation And Spectra, Planetology: Comets And Small Bodies: Surfaces And Interiors
Scientific paper
We present near-infrared spectroscopic observations (0.8-2.5 μm) of E-type asteroids. We combine these observations with visible wavelength spectra obtained by other researchers and perform Hapke theory mixing model simulations of E-type asteroid spectra in order to constrain possible compositions. Aubrites were originally suggested as the meteorite analog for the E-type asteroids because of their similar visible wavelength colors and high albedos. The designation ``E'' was originally linked with the mineral enstatite, common in aubrite meteorites. More recently, the sulfides troilite and oldhamite have been suggested as possible components of E-type asteroids. We tested the suggested compositional interpretations of aubrite meteorites and/or aubrites enhanced with sulfides. We also tested compositions of aubrites mixed with low-iron silicate minerals. We find that E types can be separated into three groups on the basis of inferred composition: ``Nysa-like'' E types are consistent with silicate mineralogy higher in iron than the mineral enstatite; ``Angelina-like'' asteroids are consistent with silicate mineralogy, including a sulfide such as oldhamite; and ``Hungaria-like'' E types are not inconsistent with aubrites. Our results indicate that some E-type asteroids may be composed of materials that are not sampled by meteorites.
Bus Schelte J.
Clark Beth Ellen
Hiroi Takahiro
McConnochie Timothy
Rivkin Andrew S.
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