Mixing in stellar radiation zones: new theoretical results

Details Mixing in stellar radiation zones: new theoretical results Mixing in stellar radiation zones: new theoretical results

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004sf2a.conf..543m&link_type=abstract

SF2A-2004: Semaine de l'Astrophysique Francaise, meeting held in Paris, France, June 14-18, 2004. Edited by F. Combes, D. Barret

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Scientific paper

We briefly recall the physical background of the rotational mixing occurring inside stellar radiation zones and its importance for stellar evolution. We describe its present modelization, its successes and its weaknesses. Next, we introduce the new theoretical results which allow us to treat the hydrodynamical processes simultaneously in the bulk of radiation zones and in the tachoclines, and we present our new prescription for the horizontal turbulent transport which has been derived from Couette-Taylor laboratory experiment. Finally, we show how to introduce self-consistently the effect of an axi or non-axisymmetric magnetic field, which may be responsible for the angular momentum transport in low-mass stars (internal gravity waves are another candidate). This research is aimed at improving the modelization of stellar interiors in the perspective of future astero and helioseismology missions such as COROT, EDDINGTON and GOLF-NG, and of new powerful ground-based instruments as ESPADON.

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