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Pre-Main Sequence Evolution of Rotating Stars in Relation with Observations of Young Clusters

Published online by Cambridge University Press:  26 May 2016

Sabatino Sofia  and
Sydney A. Barnes
Sabatino Sofia
Affiliation:
Yale University, Dept. of Astronomy, Box 208101, New Haven, CT 06520, USA
Sydney A. Barnes
Affiliation:
Univ. of Wisconsin-Madison, Dept. of Astronomy, 475 N. Charter St., Madison, WI 53703, USA and Yale University, Dept. of Astronomy, Box 208101, New Haven, CT 06520, USA

Abstract

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Assuming that pre-main sequence stars rotating at the deuterium-burning birthline as solid bodies with rates within the range observed in T-Tauri stars is an adequate initial condition to explain the rotational properties of stars in clusters of all ages, provided that appropriate evolutionary schemes are used. It is, in fact, on the evolution that most recent advances have been made, and a new paradigm has arisen. Specifically, stellar periods (as a function of mass) begin their evolution on one of two branches, and the fast rotators migrate to the slow branch through a short-lived gap. These branches represent different physical properties of the internal stellar dynamics, and are related to the type of dynamo mechanism which operates within the stars. This paradigm appears to have the potential to address several fundamental issues in stellar astronomy.

Type
Session 4 Rotation and Stellar Evolution
Information
Symposium - International Astronomical Union , Volume 215: Stellar Rotation , 2004 , pp. 419 - 428
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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