| タイトル | Overview of Vesta Mineralogy Diversity |
| 本文（外部サイト） | http://hdl.handle.net/2060/20120001854 |
| 著者（英） | Raymond, C. A.; Capria, M. T.; DeSanctis, M. C.; McSween, H.; Pieters, C. M.; Carraro, F.; Magni, G.; Mittlefehldt, D. W.; Russell, C. T.; Zambon, F.; McCord, T. B.; McFadden, L. A.; Capaccioni, F.; Frigeri, A.; Palomba, E.; Ammannito, E.; Tosi, F.; Marchi, S.; Fonte, S. |
| 著者所属（英） | NASA Johnson Space Center |
| 発行日 | 2012-01-01 |
| 言語 | eng |
| 内容記述 | 4 Vesta is known to have a surface of basaltic material through visible/near-infrared reflectance spectroscopy (1). Vesta s spectrum has strong absorption features centered near 0.9 and 1.9 m, indicative of Fe-bearing pyroxenes. The spectra of HED (howardite, eucrite and diogenite) meteorites have similar features (1). This led to the hypothesis that Vesta was the parent body of the HED clan (2,3) and the discovery of a dynamical Vesta family of asteroids (Vestoids) provides a further link between Vesta and HEDs (4). Data from the Dawn VIR (Visible InfraRed mapping Spectrometer) (5) characterize and map the mineral distribution on Vesta, strengthen the Vesta - HED linkage and provide new insights into Vesta s formation and evolution. |
| NASA分類 | Geophysics |
| レポートNO | JSC-CN-25703 |
| 権利 | Copyright, Distribution as joint owner in the copyright |
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