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Radiation-hydrodynamics simulations of surface convection in low-mass stars: connections to stellar structure and asteroseismology

Published online by Cambridge University Press:  01 April 2008

Hans-G. Ludwig ,
Elisabetta Caffau  and
A. Kučinskas
Hans-G. Ludwig
Affiliation:
Observatoire de Paris-Meudon, GEPI, 92195 Meudon Cedex, France, email: [email protected], [email protected] CIFIST Marie Curie Excellence Team, Observatoire de Paris-Meudo
Elisabetta Caffau
Affiliation:
Observatoire de Paris-Meudon, GEPI, 92195 Meudon Cedex, France, email: [email protected], [email protected]
A. Kučinskas
Affiliation:
Institute of Theoretical Physics and Astronomy, Goštauto 12, Vilnius 01108, Lithuania email: [email protected]
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Abstract

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Radiation-hydrodynamical simulations of surface convection in low-mass stars can be exploited to derive estimates of i) the efficiency of the convective energy transport in the stellar surface layers; ii) the convection-related photometric micro-variability. We comment on the universality of the mixing-length parameter, and point out potential pitfalls in the process of its calibration which may be in part responsible for the contradictory findings about its variability across the Hertzsprung-Russell digramme. We further comment on the modelling of the photometric micro-variability in HD 49933 – one of the first main COROT targets.

Keywords

convectionhydrodynamicsstars: atmospheresstars: evolutionstars: oscillations
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S252: The Art of Modeling Stars in the 21st Century , April 2008 , pp. 75 - 81
Copyright
Copyright © International Astronomical Union 2008

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