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What controls the large-scale magnetic fields of M dwarfs?

Published online by Cambridge University Press:  07 August 2014

T. Gastine ,
J. Morin ,
L. Duarte ,
A. Reiners ,
U. Christensen  and
J. Wicht
T. Gastine
Affiliation:
Max Planck Institut für Sonnensystemforschung, Max Planck Straße 2, 37191 Katlenburg-Lindau, Germany email: [email protected]
J. Morin
Affiliation:
Institut für Astrophysik, Georg-August-Universität Göttingen, Friedrich-Hund Platz, 37077 Göttingen, Germany LUPM, Université de Montpellier and CNRS, Place E. Bataillon, 34090 Montpellier, France
L. Duarte
Affiliation:
Max Planck Institut für Sonnensystemforschung, Max Planck Straße 2, 37191 Katlenburg-Lindau, Germany email: [email protected]
A. Reiners
Affiliation:
Institut für Astrophysik, Georg-August-Universität Göttingen, Friedrich-Hund Platz, 37077 Göttingen, Germany
U. Christensen
Affiliation:
Max Planck Institut für Sonnensystemforschung, Max Planck Straße 2, 37191 Katlenburg-Lindau, Germany email: [email protected]
J. Wicht
Affiliation:
Max Planck Institut für Sonnensystemforschung, Max Planck Straße 2, 37191 Katlenburg-Lindau, Germany email: [email protected]
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Abstract

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Observations of active M dwarfs show a broad variety of large-scale magnetic fields encompassing dipole-dominated and multipolar geometries. We detail the analogy between some anelastic dynamo simulations and spectropolarimetric observations of 23 M stars. In numerical models, the relative contribution of inertia and Coriolis force –estimated by the so-called local Rossby number– is known to have a strong impact on the magnetic field geometry. We discuss the relevance of this parameter in setting the large-scale magnetic field of M dwarfs.

Keywords

MHDstars: magnetic fieldstars: low-massturbulence
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S302: Magnetic Fields throughout Stellar Evolution , August 2013 , pp. 166 - 169
Copyright
Copyright © International Astronomical Union 2014 

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