ââLearning about the degree of aqueous alteration of NEOs from ...

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OUTLINE • How biased is the available sample of Carb. Chond. (CCs)? • We have studied a significant sample of historic falls • The NASA Antarctic collection opportunity: rare groups • Chondrites groups and reflectance properties in IR • Main bands and features in IR spectra of CCs – Recent findings on CM, CR, CI and CV groups. – ATR spectroscopy results from 2 to 40 m • Intrinsic chemical differences in chondrites – Collisional effects: compaction, brecciation and aqueous alteration • Implications for sample recovery in Marco-Polo-R • Preliminary results • Conclusions
WHAT WE KNOW ABOUT CARBON-RICH RICH ASTEROIDS FROM THEIR METEORITES? 253 Mathilde, NEAR Shoemaker (NASA) • Chondritic meteorites are coming from undifferentiated bodies • 15 chondrite groups identified so far (Weisber et al., 2006) – Then our overall view is highly biased! Hiroi et al. (2001) • Chemical differences among the chondrite groups suggest that each group represents rocks from a different reservoir (see e.g. Scott, 2007) • This idea has been reinforced because few chondrite breccias exist containing clasts from different chondrite groups (Bischoff et al, 2006) • Primitive asteroidal surfaces are not only brecciated, but also covered by rubble (not so important for small ones)
Page 1: “Learning about the degree of aqu
Page 5 and 6: IR SPECTROMETER IR BEAM SAMPLE haz
Page 7 and 8: ADDITIONAL STUDIED CHONDRITES • S
Page 9 and 10: MAIN ABSORPTION BANDS • The absor
Page 11 and 12: CO and CV CHONDRITE GROUPS • The
Page 13 and 14: CONCLUSIONS • Laboratory analyses

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