Circulation and turbulence in rotating stars

Details Circulation and turbulence in rotating stars Circulation and turbulence in rotating stars

Nov 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...265..115z&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 265, no. 1, p. 115-132.

Physics

490

Meridional Flow, Stellar Interiors, Stellar Physics, Stellar Rotation, Turbulence, Angular Momentum, Momentum Transfer, Stellar Composition, Stellar Models

Scientific paper

The interaction between meridian circulation and turbulence in rotating nonmagnetic stars is examined. The meridian flow is calculated and the partial differential equation which governs the transport of angular momentum is derived. Both the meridian circulation and the turbulence are determined by the loss of angular momentum, which is ascribed solely to a stellar wind. When there is no wind, the meridian flow is very weak, and it can even vanish in slow rotators. When the wind is active, it drives the circulation in order to transport angular momentum to the surface, but the advection of chemical species by this flow is partly inhibited because of the horizontal turbulence. It is concluded that, since the old population II stars are slow rotators, they do not display at their surface the original abundance of lithium.

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