Mathematics – Logic
Scientific paper
Oct 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007dps....39.3310h&link_type=abstract
American Astronomical Society, DPS meeting #39, #33.10; Bulletin of the American Astronomical Society, Vol. 39, p.478
Mathematics
Logic
Scientific paper
Systematic study of the M-asteroid population continues to reveal significant spectral and mineralogical diversity among this primarily unrelated group of main-belt asteroids. Thus far, 17 M-asteroids have been found to exhibit a variety of weak NIR absorption features indicating the presence of surficial pyroxene, olivine, or spinel. Determining the mineralogical nature of weak absorption features in NIR asteroid spectra allows tighter constraints to be placed on the geological, chemical, and thermal nature of individual asteroids, as well as identification of potential meteorite analogues. In addition, the discovery of spectral variability among the M-asteroids highlights the limitations of taxonomic identifications and interpretations.
369 Aeria and 785 Zwetana were observed at the NASA Infrared Telescope Facility (IRTF/SpeX) on April 19, 2005, UT, with the acquisition of 60 and 30 spectra, respectively. 369 Aeria exhibits weak 0.9- and 1.9-micron absorption features on an overall reddish NIR spectrum that exhibits similarities to mesosiderite spectra. Spectra were obtained across two-thirds of a rotation of the asteroid, which revealed systematic variations of the 0.9- and 1.9-micron absorptions. These band parameters change systematically with rotation of the asteroid and suggest a small, but measurable, change in orthopyroxene chemistry across the surface of the asteroid. Band Area Ratio (BAR) values for 369 Aeria are larger than 2.8, suggesting pyroxene is the significant mafic silicate on Aeria's surface. The weakness of the absorption features also suggest a significant abundance of surface metal, which weakens pyroxene absorption features.
NIR spectra of 785 Zwetana exhibit a broad, weak absorption beyond 1.30-microns without a corresponding 1-micron feature. Analysis suggests that the spectrally active phase on the surface of 785 Zwetana is spinel, which also suggests the presence of CAIs and a CO/CV-chondrite-like meteoritic analogue. This research is supported by NASA Planetary Astronomy Program Grant NNG05GH01G.
Gaffey Michael J.
Hardersen Paul Scott
Kumar Sanjeev
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