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Synthetic activity indicators for M-type dwarf stars

Published online by Cambridge University Press:  09 September 2016

Sven Wedemeyer  and
Hans-Günter Ludwig
Sven Wedemeyer
Affiliation:
Institute of Theoretical Astrophysics, University of Oslo, Postboks 1029 Blindern, N-0315 Oslo, Norway email: sven.wedemeyer@astro.uio.no
Hans-Günter Ludwig
Affiliation:
ZAH-Landessternwarte, University of Heidelberg, Heidelberg, Germany email: hludwig@lsw.uni-heidelberg.de
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Abstract

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Here, we present a set of time-dependent 3D RMHD simulations of a M-dwarf star representative of AD Leo, which extend from the upper convection zone into the chromosphere. The 3D model atmospheres are characterized by a very dynamic and intermittent structure on small spatial and temporal scales and a wealth of physical processes, which by nature cannot be described by means of 1D static model atmospheres. Artificial observations of these models imply that a combination of complementary diagnostics such as Ca II lines and the continuum intensity from UV to millimeter wavelengths, probe various properties of the dynamics, thermal and magnetic structure of the photosphere and the chromosphere and thus provide measures of stellar activity, which can be compared to observations. The complicated magnetic field structure and its imprint in synthetic diagnostics may have important implications for the understanding and characterization of stellar activity and with it possibly for the evaluation of planetary habitability around active M-dwarf stars.

Keywords

(magnetohydrodynamics:) MHDradiative transferstars: activitystars: atmospheresstars: chromospheresstars: magnetic fields
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S320: Solar and Stellar Flares and their Effects on Planets , August 2015 , pp. 303 - 308
Copyright
Copyright © International Astronomical Union 2016 

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