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Rotation of Pre-Main Sequence Stars from High S/N Spectroscopy

Published online by Cambridge University Press:  19 July 2016

J. Bouvier
J. Bouvier*
Affiliation:
Institut d'Astrophysique, 98 bis bd Arago, F-75014 Paris

Abstract

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Until 1980, only a handful of low-mass, active pre-main sequence (pms) stars had known rotation velocities (vsini) /1/. Since then, increasingly sensitive detectors coupled to large telescopes led to high–resolution (a few 104) spectroscopic studies of these faint stars (mv = 10–13), with S/N ratio of the order of 100. The measurement of vsini for large samples of pms stars that resulted brought new insights on various pressing questions related to stellar formation and early stellar evolution : how do the rotation rates of pms stars compare with those expected from models of stellar formation ? how does the stellar angular momentum change during pms evolution ? is pms activity linked with rotation as would be expected if activity were triggered by magnetic processes ?

Type
II. Pre-Main-Sequence Stars
Information
Symposium - International Astronomical Union , Volume 132: The Impact of Veryhigh S/N Spectroscopy on Stellar Physics , 1988 , pp. 95 - 98
Copyright
Copyright © Kluwer 1988 

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