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Three Single Stars (See How They Spin)

Published online by Cambridge University Press:  26 May 2016

Paul Charbonneau
Paul Charbonneau*
Affiliation:
Département de Physique, Université de Montréal, CP 6128 Centre-Ville, Montreal (Qc), H3C 3J7 CANADA

Abstract

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I describe three key moments in the rotational evolution of three single stars, chosen to illustrate the richness and complexity of the interaction between rotation and magnetic fields. I then piece together two general scenarii for the rotational evolution of early-type and late-type stars, in which the “fossil” magnetic field inherited by a star from its formative years basically sets its subsequent rotational fate. Since no one has yet offered a convincing scenario according to which a star could somehow get rid of its primordial fossil field, the inescapable conclusion is that magnetic fields cannot be neglected in modelling rotation, and that “rotational evolution” should really be thought of as “magnetorotational evolution”.

Type
Session 3 Rotation, Solar and Stellar Physics
Information
Symposium - International Astronomical Union , Volume 215: Stellar Rotation , 2004 , pp. 366 - 375
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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