Mathematics – Logic
Scientific paper
May 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003dps....35.2205c&link_type=abstract
American Astronomical Society, DPS meeting #35, #22.05; Bulletin of the American Astronomical Society, Vol. 35, p.955
Mathematics
Logic
1
Scientific paper
What are the X-types made of? How would knowledge of their composition change our picture of the geological structure of the asteroid regions? X-types are important in the main belt, yet we do not understand their composition or meteorite linkage. This is an outstanding problem in asteroid-meteorite studies, because X-types comprise approximately 20% of the inner main belt (Tholen and Barucci 1989; Bus 1999). We have conducted a program of infrared (0.8-2.5microns) observations aimed at determining mineralogy without albedo information. Because X-types are spectrally like E, M, and P-type asteroids, we observed 18 X-types, 5 E-types, 8 M-types, and 4 P-types. This is the first focused study of XEMP asteroids. In this paper, we present a compositional analysis of the new spectral data.
What we call XEMPs are asteroids identified as ambiguous on the basis of their visible spectral properties only (Zellner et al. 1985; Tholen 1984; Bus and Binzel 2002). By convention (Bowell et al. 1978; Tholen and Barucci 1989), X-types with measured geometric albedos are classified into E, M, or P-types, where E-types (designated ``E" based on their possible link with enstatite meteorites) are high-albedo objects, P-types are low-albedo objects (there are no meteorite analogs for these objects), and M-types (designated ``M" based on their possible link with metallic meteorites) are intermediate. Bus and Binzel (2002) found subtle features in X-class spectra in a high resolution survey.
We have regrouped XEMP spectra for a reanalysis of the extended wavelength coverage now available (0.3-2.5 microns). When continuum slope is removed, we find distinct 0.9 micron bands at the level of 2-5% in many of our XEMP objects. We also find consistent wavelength maxima near 1.5 microns, and hints of 2.0 micron bands in some objects. Our preliminary findings suggest that new mineralogy-based groupings may be called for, breaking down the old albedo-based E, M, and P-type designations.
We gratefully acknowledge funding support from the Research Corporation.
Bus Schelte J.
Clark Beth Ellen
Rivkin Andrew S.
Sanders James
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