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Differential Rotation in Stars with Convection Zones

Published online by Cambridge University Press:  12 April 2016

Peter A. Gilman
Peter A. Gilman*
Affiliation:
High Altitude Observatory, National Center for Atmospheric Research, Boulder, Colorado 80307/USA

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The topic I was originally assigned for this colloquium was “Generation of Non Thermal, Non Oscillatory Motions”. Being basically a fluid dynamicist, at first I thought this meant I was supposed to talk about the origin of motions which are not thermally driven, i.e., I should not talk about convection. But then I realized all that was meant was that I was to talk about bulk fluid motions, rather than the molecular “thermal” motion of stellar gas that defines its temperature. Obviously the original question was posed by a stellar spectroscopist! Having surmounted that small semantic hurdle, I began to think about all the ways circulatory motions might be generated in a star. All manner of fluid dynamical instabilities come to mind--not only convective instability, but also barotropic or inertial, baroclinic, Kelvin-Helmholz, Rayleiqh-Taylor, Goldreich-Shubert, Solberg-Hoiland, etc. The list is large, overlapping, I am sure confusing to an observer (and to many a theoretician). Then there are Eddington-Sweet currents, and several additional motions arising from the presence of magnetic fields--fields which give rise to magnetic buoyancy of flux tubes, and large collection of magnetohydrodynamic instabilities.

Type
1. The Pyhsical Origin of Turbulence
Information
International Astronomical Union Colloquium , Volume 51: Stellar Turbulence , 1980 , pp. 19 - 37
Copyright
Copyright © Springer-Verlag 1980

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