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Onward from solar convection to dynamos in cores of massive stars

Published online by Cambridge University Press:  12 August 2011

Juri Toomre
Juri Toomre*
Affiliation:
JILA & Dept of Astrophysical and Planetary Sciences, University of Colorado, Boulder, CO 80309-0440, USA email: [email protected]
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Abstract

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We reflect upon a few of the research challenges in stellar convection and dynamo theory that are likely to be addressed in the next five or so years. These deal firstly with the Sun and continuing study of the two boundary layers at the top and bottom of its convection zone, namely the tachocline and the near-surface shear layer, both of which are likely to have significant roles in how the solar dynamo may be operating. Another direction concerns studying core convection and dynamo action within the central regions of more massive A, B and O-type stars, for the magnetism may have a key role in controlling the winds from these stars, thus influencing their ultimate fate. Such studies of the interior dynamics of massive stars are becoming tractable with recent advances in codes and supercomputers, and should also be pursued with some vigor.

Keywords

Sun: tachoclineSun: near-surface shear layerSun: dynamo actionstars: massive star convection
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S271: Astrophysical Dynamics: From Stars to Galaxies , June 2010 , pp. 347 - 352
Copyright
Copyright © International Astronomical Union 2011

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