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

Published online by Cambridge University Press:  26 May 2016

Robert D. Mathieu
Robert D. Mathieu*
Affiliation:
University of Wisconsin, Department of Astronomy, Madison WI 53706 USA

Abstract

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Major photometric monitoring campaigns of star-forming regions in the past decade have provided rich rotation period distributions of pre-main-sequence stars. The rotation periods span more than an order of magnitude in period, with most falling between 1 and 10 days. Thus the broad rotation period distributions found in 100 Myr clusters are already established by an age of 1 Myr. The most rapidly rotating stars are within a factor of 2-3 of their critical velocities; if angular momentum is conserved as they evolve to the ZAMS, these stars may come to exceed their critical velocities. Extensive efforts have been made to find connections between stellar rotation and the presence of protostellar disks; at best only a weak correlation has been found in the largest samples. Magnetic disk-locking is a theoretically attractive mechanism for angular momentum evolution of young stars, but the links between theoretical predictions and observational evidence remain ambiguous. Detailed observational and theoretical studies of the magnetospheric environments will provide better insight into the processes of pre-main-sequence stellar angular momentum evolution.

Type
Session 1 Observations of Rotating Stars
Information
Symposium - International Astronomical Union , Volume 215: Stellar Rotation , 2004 , pp. 113 - 122
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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