The Nature of M-Class Asteroids from 3-μm Observations

A. S. Rivkin, E. S. Howell, L. A. Lebofsky, B. E. Clark, D. T. Britt

Research output: Contribution to journalArticlepeer-review

122 Scopus citations

Abstract

We have spectrophotometrically observed twenty M-class asteroids in the 1.2- to 3.5-μm region, sixteen of them for the first time. When we combined these with earlier surveys by Rivkin et al. (1995) and Jones et al. (1990) for a total of 27 asteroids, we find that over 35% of them have absorption features at 3 μm diagnostic of water of hydration. This absorption feature is inconsistent with these M-class asteroids being primarily Fe-Ni metal, which would be expected if they were remnant cores of disrupted differentiated objects. We also find that large (D>65 km) M asteroids are very likely to be hydrated (75%), while small (D<65 km) M asteroids are very unlikely to be hydrated (10%). We believe the interpretation most consistent with all data (astronomical, meteoritical, and geochemical modeling) holds the large M-class asteroids to be relatively primitive material perhaps akin to enstatite chondrites or salt-rich carbonaceous chondrites, with the iron meteorites found on Earth perhaps deriving from the smaller, anhydrous M asteroids. In keeping with Rivkin et al. (1995), we place the hydrated M asteroids in the separate W class.

Original languageEnglish (US)
Pages (from-to)351-368
Number of pages18
JournalIcarus
Volume145
Issue number2
DOIs
StatePublished - Jun 2000
Externally publishedYes

Keywords

  • Asteroids
  • Composition
  • Infrared observations
  • Spectrophotometry

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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