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The Interaction of Rotation with Convection

Published online by Cambridge University Press:  12 April 2016

Bernard R. Durney
Bernard R. Durney*
Affiliation:
High Altitude Observatory, National Center for Atmospheric Research*, Boulder, Colo., U.S.A.

Abstract

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The equations for a rotating convective spherical shell are solved in the Herring approximation as an initial value problem. The main results are

  • (1) The most unstable modes (those that maximize the heat flux) correspond to convective cells stretching from pole to pole.

  • (2) The calculations of the Reynolds stresses show transport of angular momentum towards the equator. That is, differential rotation sets in with equatorial acceleration.

  • (3) The convective heat transport is maximum at the equator. This would give rise to an equator-pole flux difference.

  • (4) If convection is non-axisymmetric (as in the most unstable modes) there are no time independent solutions. The time dependence is oscillatory and of the form ωt + mφ.

Type
Part I / The Effects of Rotation on Stellar Interiors and Evolution
Information
International Astronomical Union Colloquium , Volume 4: Stellar Rotation , 1970 , pp. 30 - 36
Copyright
Copyright © Reidel 1970

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