On rotationally driven meridional flows in stars

Details On rotationally driven meridional flows in stars On rotationally driven meridional flows in stars

2002-03-21

arxiv.org/abs/astro-ph/0203382v1

Mon.Not.Roy.Astron.Soc. 335 (2002) 707

Astronomy and Astrophysics

Astrophysics

5 pages, submitted to MNRAS Letters

Scientific paper

10.1046/j.1365-8711.2002.05662.x

A quasi-steady state model of the consequences of rotation on the hydrodynamical structure of a stellar radiative zone is derived, by studying in particular the role of centrifugal and baroclinic driving of meridional motions in angular-momentum transport. This nonlinear problem is solved numerically assuming axisymmetry of the system, and within some limits, it is shown that there exist simple analytical solutions. The limit of slow rotation recovers Eddington-Sweet theory, whereas it is shown that in the limit of rapid rotation, the system settles into a geostrophic equilibrium. The behaviour of the system is found to be controlled by one parameter only, linked to the Prantl number, the stratification and the rotation rate of the star.

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