Investigating The Spectral Diversity Of V-type Asteroids In The Inner Main Belt

Details Investigating The Spectral Diversity Of V-type Asteroids In The Inner Main Belt Investigating The Spectral Diversity Of V-type Asteroids In The Inner Main Belt

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008dps....40.6002m&link_type=abstract

American Astronomical Society, DPS meeting #40, #60.02; Bulletin of the American Astronomical Society, Vol. 40, p.508

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Spectroscopic (Binzel & Xu, 1993), dynamical (Zappala et al., 1990) and morphological (Thomas et al., 1997) evidence suggests that the Vestoids are a population of basaltic asteroids that were ejected from the surface of Vesta as a consequence of a large family-forming impact. Over time these fragments have migrated via the Yarkovsky effect (Bottke et al., 2001) and interaction with secular resonances (Carruba et al., 2005) to large orbital distances from Vesta. However, Nesvorny et al. (2008) suggest that regions of high (i > 9 deg.) and low inclination (i < 4 deg.) in the inner Main Belt cannot be populated by a significant number of Vestoids. Thus, the recent identification of numerous V-type asteroids in these regions (Moskovitz et al., 2008; Roig & Gil-Hutton, 2006) raises two interesting possibilities: (1) they originated from a differentiated parent body other than Vesta, or (2) they originated from Vesta before the primary family forming impact and before the Late Heavy Bombardment when resonance sweeping dynamically excited the Main Belt. The possibility of a unique parent body or an older surface implies that the surface mineralogy of these objects may be distinct from that of "ordinary” Vestoids. In consideration of these issues we present new spectra and analysis for a variety of V-type asteroids throughout the inner Main Belt (a < 2.5 AU) with a particular focus on objects that have large values of delta-v (Zappala et al., 1996) relative to Vesta. Our analysis includes a search for trends in the spectral properties of these objects as a function of orbital distance from Vesta and an attempt to link these spectral properties to the petrology of meteorite samples using both band analysis techniques (Burbine et al., 2007) and MGM analysis (Sunshine et al., 1990). This work is supported by a NASA GSRP fellowship.

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