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Near-surface stellar magneto-convection: simulations for the Sun and a metal-poor solar analog

Published online by Cambridge University Press:  01 November 2008

Matthias Steffen ,
H.-G. Ludwig  and
O. Steiner
Matthias Steffen
Affiliation:
Astrophysikalisches Institut Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany, email: msteffen@aip.de
H.-G. Ludwig
Affiliation:
GEPI, Observatoire de Paris, CNRS, Université Paris Diderot, 92195 Meudon Cedex, France
O. Steiner
Affiliation:
Kiepenheuer-Institut für Sonnenphysik, Schöneckstrasse 6, D-79104 Freiburg, Germany
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Abstract

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We present 2D local box simulations of near-surface radiative magneto-convection with prescribed magnetic flux, carried out with the MHD version of the CO5BOLD code for the Sun and a solar-like star with a metal-poor chemical composition (metal abundances reduced by a factor 100, [M/H] = −2). The resulting magneto-hydrodynamical models can be used to study the influence of the metallicity on the properties of magnetized stellar atmospheres. A preliminary analysis indicates that the horizontal magnetic field component tends to be significantly stronger in the optically thin layers of metal-poor stellar atmospheres.

Keywords

Convection – Sun: atmosphere – stars: atmospheres – MHD
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S259: Cosmic Magnetic Fields: From Planets, to Stars and Galaxies , November 2008 , pp. 233 - 234
Copyright
Copyright © International Astronomical Union 2009

References

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