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Convection and dynamo action in B stars

Published online by Cambridge University Press:  12 August 2011

Kyle C. Augustson ,
Allan S. Brun  and
Juri Toomre
Kyle C. Augustson
Affiliation:
JILA & APS, University of Colorado, 440 UCB, Boulder, CO, 80309-0440, USA
Allan S. Brun
Affiliation:
UMR AIM CEA-CNRS-Univ. P7 CEA Saclay, 91191 Gif-sur-Yvette Cedex, France
Juri Toomre
Affiliation:
JILA & APS, University of Colorado, 440 UCB, Boulder, CO, 80309-0440, USA
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Abstract

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Main-sequence massive stars possess convective cores that likely harbor strong dynamo action. To assess the role of core convection in building magnetic fields within these stars, we employ the 3-D anelastic spherical harmonic (ASH) code to model turbulent dynamics within a 10 M⊙ main-sequence (MS) B-type star rotating at 4 Ω⊙. We find that strong (900 kG) magnetic fields arise within the turbulence of the core and penetrate into the stably stratified radiative zone. These fields exhibit complex, time-dependent behavior including reversals in magnetic polarity and shifts between which hemisphere dominates the total magnetic energy.

Keywords

stars: early typerotationmagnetic fields
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S271: Astrophysical Dynamics: From Stars to Galaxies , June 2010 , pp. 361 - 362
Copyright
Copyright © International Astronomical Union 2011

References

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