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Rotational Evolution of Intermediate and Low Mass Main Sequence Stars

Published online by Cambridge University Press:  26 May 2016

John R. Stauffer
John R. Stauffer*
Affiliation:
SIRTF Science Center, Keith-Spalding Building, MS 314-6, Caltech, Pasadena, CA 91125

Abstract

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Bob Kraft (1967) showed that there is a break in the mean rotational velocity of stars at about spectral type F5, with more massive stars generally being rapid rotators and less massive stars generally being slow rotators. He also showed that in the late F spectral range at least, there is an evolution with time on the main sequence, with younger F stars being more rapidly rotating. Kraft's observational database extended only to about one solar mass due to the sensitivy limitations of photographic plates. Modern observations of low mass stars in open clusters, extending down in mass to nearly the hydrogen burning mass limit in a few clusters, have since been used to show that rotational spindown is the common feature of stars less massive than the sun but that there is a wide spread in rotational velocities when stars arrive on the ZAMS. I will review what is known empirically concerning the rotational velocities of intermediate and low mass field stars, using the open cluster data to place the field star observations in context.

Type
Session 1 Observations of Rotating Stars
Information
Symposium - International Astronomical Union , Volume 215: Stellar Rotation , 2004 , pp. 127 - 135
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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