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Rotating Stellar Interiors (Review Paper)

Published online by Cambridge University Press:  23 September 2016

Robert Connon Smith
Robert Connon Smith*
Affiliation:
Astronomy Centre, University of Sussex, Falmer, Brighton BN1 9QH, U.K.

Abstract

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Rotation has two main qualitative effects on the structure of a star: it distorts the shape and it reduces the total luminosity. The luminosity depends only on the total angular momentum but the shape, and so the observable properties, depends on the internal distribution of angular momentum. The expected distribution, even for main-sequence stars, is an unsolved problem. Redistribution of angular momentum can occur as a result of large-scale circulation currents, instabilities and magnetic stresses and there may be no steady state. If shear instabilities are dominant, then stars may rotate nearly uniformly. Studies of non-radial oscillations might perhaps eventually lead to a direct probing of the internal angular momentum distribution by the methods now being used to study the internal rotation of the Sun. Differential rotation near the surface would probably give rise to turbulent motions, which could generate the mechanical energy flux which seems to be a necessary input to the winds in hot stars.

Type
IIB. The Underlying Stars: Theory
Information
International Astronomical Union Colloquium , Volume 92: Physics of Be Stars , August 1987 , pp. 123 - 146
Copyright
Copyright © Cambridge University Press 1987

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