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Stellar rotation and mixing

Published online by Cambridge University Press:  25 May 2016

Jean-Paul Zahn
Jean-Paul Zahn*
Affiliation:
Département d'Astrophysique Stellaire et Galactique, Observatoire de Paris, 92195 Meudon, France

Abstract

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Many observations indicate that some mixing occurs in stellar radiation zones: in massive stars, chemical elements resulting from nuclear burning in the core are detected at the surface, and in solar-type stars lithium is depleted with age. Since all mixing processes transport also momentum, the depletion of lithium should be linked with the loss of angular momentum through the stellar wind, and there are indeed signs of such a correlation in the behavior of tidally-locked binaries. Moreover, any transport process leaves its signature in the internal rotation profile, and this can help greatly in its identification. After reviewing the main transport mechanisms which have been considered so far, our present conclusion is that the uniform rotation observed in the radiative interior of the Sun is probably achieved by the action of internal waves emitted at the base of the convective envelope. It remains to be verified whether these waves contribute directly to the mixing, or whether they act only through the shaping of the rotation profile, which in turn determines the mixing through meridian circulation and turbulent diffusivity.

Type
Part II: Internal structure and rotation. Seismic inversions
Information
Symposium - International Astronomical Union , Volume 181: Sounding Solar and Stellar Interiors , 1997 , pp. 175 - 188
Copyright
Copyright © Kluwer 1997 

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