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Photospheric magnetoconvection

Published online by Cambridge University Press:  01 August 2006

Robert Cameron ,
Alexander Vögler  and
Manfred Schüssler
Robert Cameron
Affiliation:
Max-Planck Instute for Solar System Research, Katlenburg-Lindau, Germanycameron@mps.mpg.de
Alexander Vögler
Affiliation:
Max-Planck Instute for Solar System Research, Katlenburg-Lindau, Germanycameron@mps.mpg.de
Manfred Schüssler
Affiliation:
Max-Planck Instute for Solar System Research, Katlenburg-Lindau, Germanycameron@mps.mpg.de
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Abstract

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Magnetic fields, convective motions and radiative energy transport all strongly influence each other in the solar photosphere. Attempts to understand, at a quantitative level, the diverse phenomona seen in the photosphere have relied on increasingly powerful computers since the 1980's. This approach has been remarkably successful and some recent examples, particularly cases where all three ingredients are important, will be discussed.

Keywords

Convectionmagnetic fieldsradiative transferSun: photosphere
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S239: Convection in Astrophysics , August 2006 , pp. 475 - 481
Copyright
Copyright © International Astronomical Union 2007

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