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On dynamo action in the giant star Pollux: first results

Published online by Cambridge University Press:  07 August 2014

Ana Palacios  and
Allan Sacha Brun
Ana Palacios
Affiliation:
LUPM, Université Montpellier II, Place Eugène Bataillon cc -0072, F-34095, Montpellier cedex 5, France email: ana.palacios@univ-montp2.fr Laboratoire AIM Paris-Saclay, CEA/Irfu Université Paris-Diderot CNRS/INSU, 91191 Gif-sur-Yvette, France email: sacha.brun@cea.fr
Allan Sacha Brun
Affiliation:
Laboratoire AIM Paris-Saclay, CEA/Irfu Université Paris-Diderot CNRS/INSU, 91191 Gif-sur-Yvette, France email: sacha.brun@cea.fr
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Abstract

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We present preliminary results of a 3D MHD simulation of the convective envelope of the giant star Pollux for which the rotation period and the magnetic field intensity have been measured from spectroscopic and spectropolarimetric observations. This giant is one of the first single giants with a detected magnetic field, and the one with the weakest field so far. Our aim is to understand the development and the action of the dynamo in its extended convective envelope.

References

Aurière, M., Wade, G., Konstantinova-Antova, R.et al. 2009, A&A, 504, 231Google Scholar
Brun, A. S. & Palacios, A. 2009, ApJ, 702, 1078CrossRefGoogle Scholar
Brun, A. S., Miesch, M. S., & Toomre, J. 2004, ApJ, 614, 1073CrossRefGoogle Scholar
Featherstone, et al. 2014, in preparationGoogle Scholar