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On Rotationally Driven Meridional Flows in Stars

Published online by Cambridge University Press:  26 May 2016

P. Garaud
P. Garaud*
Affiliation:
DAMTP, Silver Street, University of Cambridge, CB39EW Cambridge

Abstract

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The first entirely self-consistent 2D model of rotational mixing in a stellar radiative zone is presented. This nonlinear problem is solved numerically assuming axisymmetry of the system. The dynamical behaviour of a rotating star is found to be controlled by one parameter only, the ratio of the Eddington-Sweet timescale to the viscous timescale. In the quasi-steady state, the limit of slow rotation recovers Eddington-Sweet theory, whereas in the limit of rapid rotation, the system settles into a centrifugal equilibrium. The evolution of the dynamical structure of the star undergoing spin-down is then studied, and the relevance of these findings to observations of rotational mixing is discussed.

Type
Session 3 Rotation, Solar and Stellar Physics
Information
Symposium - International Astronomical Union , Volume 215: Stellar Rotation , 2004 , pp. 348 - 353
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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