EAS Publications Series
Volume 26, 2007Stellar Evolution and Seismic Tools for Asteroseismology - Diffusive Processes in Stars and Seismic Analysis
|Page(s)||65 - 78|
|Published online||20 June 2007|
C.W. Straka, Y. Lebreton and M.J.P.F.G. Monteiro (eds)
EAS Publications Series, 26 (2007) 65-78
Advances in Secular Magnetohydrodynamics of Stellar Interiors Dedicated to Asteroseismic Spatial Missions
CEA/DSM/DAPNIA/Service d'Astrophysique, CEA/Saclay; AIM-Unité Mixte de Recherche CEA-CNRS-Université Paris VII, UMR 7158, 91191 Gif-sur-Yvette Cedex, France
2 LUTH, Observatoire de Paris, 5 place Jules Janssen, 92195 Meudon Cedex, France
3 Observatoire de Genève, 51 chemin des Maillettes, 1290 Sauverny, Switzerland
4 Institut d'Astrophysique et de Géophysique, Université de Liège, Allée du 6 Août, 17 1/14 (B5C), 4000 Liège 1 (Sart Tilman), Belgium
5 GRAAL, Université de Montpellier II, Place Eugène Bataillon, 34095 Montpellier Cedex 05, France
6 Institut d'Astronomie et d'Astrophysique, Université Libre de Bruxelles, Campus de la Plaine, Boulevard du Triomphe, CP 226, 1050 Bruxelles, Belgium
7 LATT, Observatoire Midi-Pyrénées; 14 avenue Edouard Belin, 31400 Toulouse, France
With the first light of COROT, the preparation of KEPLER and the future helioseismology spatial projects such as GOLF-NG, a coherent picture of the evolution of rotating stars from their birth to their death is needed. We describe here the modelling of the macroscopic transport of angular momentum and matter in stellar interiors that we have undertaken to reach this goal. First, we recall in detail the dynamical processes that are driving these mechanisms in rotating stars and the theoretical advances we have achieved. Then, we present our new results of numerical simulations which allow us to follow in 2D the secular hydrodynamics of rotating stars, assuming that anisotropic turbulence enforces a shellular rotation law. Finally, we show how this work is leading to a dynamical vision of the Hertzsprung-Russel diagram with the support of asteroseismology and helioseismology, seismic observables giving constraints on the modelling of the internal transport and mixing processes. In conclusion, we present the different processes that should be studied in the near future to improve our description of stellar radiation zones.
© EAS, EDP Sciences, 2007
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