The formation and evolution of ordinary chondrite parent bodies

Pierre Vernazza, Brigitte Zanda, Tomoki Nakamura, Edward Scott, Sara Russell

Research output: Chapter in Book/Report/Conference proceedingChapterpeer-review

19 Citations (Scopus)


Ordinary chondrites (OCs) are by far the most abundant meteorites (80% of all falls). Their origin has long been the matter of a heated debate. About 30 years ago (e.g., Pellas, 1988), it was proposed that OCs should originate from S-type bodies (the most abundant asteroid spectral types in the inner part of the asteroid belt), but the apparent discrepancy between S-type asteroid and OC reflectance spectra generated what was known as the S-type/OC conundrum. This paradox has gradually been resolved over the years. It is now understood that space weathering processes are responsible for the spectral mismatch between S-type bodies and OCs. Furthermore, both telescopic observations and the first asteroid sample return mission (Hayabusa) indicate that most S-type bodies have mineralogies similar to those of OCs. Importantly, the S-type/OC link, which has remained sterile for more than 30 years, has been delivering fundamental constraints on the formation and evolution of planetesimals over the recent years.

Original languageEnglish
Title of host publicationAsteroids IV
PublisherUniversity of Arizona Press
Number of pages18
ISBN (Electronic)9780816532186
ISBN (Print)9780816532131
Publication statusPublished - 2015 Jan 1


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