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Angular Momentum Transport and Mixing by Magnetic Fields

Published online by Cambridge University Press:  26 May 2016

H. C. Spruit
H. C. Spruit*
Affiliation:
Max-Planck Institut für Astrophysik, Postfach 1317, 85741 Garching, Germany

Abstract

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Magnetic fields can be created in stably stratified (non-convective) layers in a differentially rotating star. A magnetic instability in the toroidal field (wound up by differential rotation) replaces the role of convection in closing the field amplification loop. A dynamo model is developed from these ingredients, and applied to the problem of angular momentum transport in stellar interiors. It produces a predominantly horizontal field. The process is found to be more effective in transporting angular momentum than the known hydrodynamic mechanisms, with the possible exception of transport by internal gravity waves.

Information

Type
Session 3 Rotation, Solar and Stellar Physics
Information
Symposium - International Astronomical Union , Volume 215: Stellar Rotation , 2004 , pp. 356 - 365
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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