Rotation of Low Mass Pre-Main Sequence Stars

Details Rotation of Low Mass Pre-Main Sequence Stars Rotation of Low Mass Pre-Main Sequence Stars

Jul 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005sfet.confe..24h&link_type=abstract

"Star Formation in the Era of Three Great Observatories, meeting abstracts from the conference held July 13-15, 2005 in Cambridg

Physics

Scientific paper

Photometric monitoring campaigns have yielded rotation periods, with a typical accuracy of about 1%, for nearly 2000 pre-main sequence stars of low mass in nearby clusters and associations. When combined with stellar radii, these data yield the average specific angular momentum (j) of the surface layer of each star. There are now sufficient data that we can assess on a quantitative statistical basis how the frequency distribution of j depends on mass and age. Empirical results will be presented and an interpretation in terms of the canonical theory of disk locking proposed. The implications of these results for accretion disk lifetimes and for the interpretation of X-ray observations will be briefly summarized.

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