Rotation rates of late-type stars in open clusters

Details Rotation rates of late-type stars in open clusters Rotation rates of late-type stars in open clusters

Feb 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001noao.prop..259b&link_type=abstract

NOAO Proposal ID #2001A-0259

Computer Science

Scientific paper

The study of stellar rotation provides unique insights into the interiors of stars, their magnetic fields, the winds that blow from their surfaces, and the interaction between the young star and its circumstellar disk. Sophisticated theoretical models already developed make definite and testable predictions of how the rotation rates of stars change with mass and age. At the present time, the models are ahead of the data because sufficient observations are not available to constrain them. But if observations do become available to compare with theory, they are likely to lead to fundamental insights about both the interiors and immediate exteriors of stars, including star-disk interaction. The most urgent need at the present time is for measurements of stars with ages between those of the young (<=100 Myr) and the Hyades (<=600 Myr) clusters and beyond. We therefore propose to determine, from precise CCD photometry, rotation periods for a group of solar-type (G, K and M type) stars in the 350 Myr-old open cluster NGC 6494 and the 900 Myr-old cluster NGC 5822.

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