| Article ID | Journal | Published Year | Pages | File Type |
|---|---|---|---|---|
| 1774232 | Icarus | 2010 | 10 Pages |
Abstract
We observe spectral variations across Vesta' surface that can be interpreted as variations of either the pyroxene composition, or the effect of surface aging. We compare Vesta's 2 μm absorption band to that of howardite-eucrite-diogenite (HED) meteorites that are thought to originate from Vesta, and establish particular links between specific regions and HED subclasses. The overall composition is found to be mostly compatible with howardite meteorites, although a small area around 180°E longitude could be attributed to a diogenite-rich spot. We finally focus our spectral analysis on the characteristics of Vesta's bright and dark regions as seen from Hubble Space Telescope's visible and Keck-II's near-infrared images.
Related Topics
Physical Sciences and Engineering
Earth and Planetary Sciences
Space and Planetary Science
Authors
Benoît Carry, Pierre Vernazza, Christophe Dumas, Marcello Fulchignoni,