Convection and dynamo action in B stars

Details Convection and dynamo action in B stars Convection and dynamo action in B stars

2010-11-03

arxiv.org/abs/1011.1016v1

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

2 pages, 1 figure; IAU symposium 271, Astrophysical Dynamics: From Galaxies to Stars

Scientific paper

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 solar mass main-sequence (MS) B-type star rotating at 4 times the solar rate. 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.

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