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Turbulence and magnetic spots at the surface of hot massive stars

Published online by Cambridge University Press:  26 August 2011

Matteo Cantiello ,
Jonathan Braithwaite ,
Axel Brandenburg ,
Fabio Del Sordo ,
Petri Käpylä  and
Norbert Langer
Matteo Cantiello
Affiliation:
Argelander-Institut für Astronomie der Universität Bonn, Auf dem Hügel 71, D–53121 Bonn, Germany email: cantiello@astro.uni-bonn.de
Jonathan Braithwaite
Affiliation:
Argelander-Institut für Astronomie der Universität Bonn, Auf dem Hügel 71, D–53121 Bonn, Germany email: cantiello@astro.uni-bonn.de
Axel Brandenburg
Affiliation:
NORDITA, AlbaNova University Center, Roslagstullsbacken 23, SE-10691 Stockholm, Sweden Department of Astronomy, AlbaNova University Center, Stockholm University, SE–10691 Stockholm, Sweden
Fabio Del Sordo
Affiliation:
NORDITA, AlbaNova University Center, Roslagstullsbacken 23, SE-10691 Stockholm, Sweden Department of Astronomy, AlbaNova University Center, Stockholm University, SE–10691 Stockholm, Sweden
Petri Käpylä
Affiliation:
NORDITA, AlbaNova University Center, Roslagstullsbacken 23, SE-10691 Stockholm, Sweden Department of Physics, Gustaf Hällströmin katu 2a (PO Box 64), FI-00014, University of Helsinki, Finland
Norbert Langer
Affiliation:
Argelander-Institut für Astronomie der Universität Bonn, Auf dem Hügel 71, D–53121 Bonn, Germany email: cantiello@astro.uni-bonn.de
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Abstract

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Hot luminous stars show a variety of phenomena in their photospheres and in their winds which still lack clear physical explanations at this time. Among these phenomena are non-thermal line broadening, line profile variability (LPVs), discrete absorption components (DACs), wind clumping and stochastically excited pulsations. Cantiello et al. (2009) argued that a convection zone close to the surface of hot, massive stars, could be responsible for some of these phenomena. This convective zone is caused by a peak in the opacity due to iron recombination and for this reason is referred to as the “iron convection zone” (FeCZ). 3D MHD simulations are used to explore the possible effects of such subsurface convection on the surface properties of hot, massive stars. We argue that turbulence and localized magnetic spots at the surface are the likely consequence of subsurface convection in early type stars.

Keywords

Convectionhydrodynamicswavesstars: activitystars: atmospheresstars: evolutionstars: magnetic fieldsstars: spotsstars: windsoutflows
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S273: The Physics of Sun and Star Spots , August 2010 , pp. 200 - 203
Copyright
Copyright © International Astronomical Union 2011

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