Kyle C. Augustson, Allan S. Brun, Juri Toomre
Published 2010-11-03Version 1
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.
Comments: 2 pages, 1 figure; IAU symposium 271, Astrophysical Dynamics: From Galaxies to Stars
Convection, rotation, and magnetic activity of solar-like stars from asteroseismology
Solar Dynamics, Rotation, Convection and Overshoot
Convection and convective overshooting in stars more massive than 10 $M_\odot$
![QR code for arXiv:1011.1016 [astro-ph.SR]](http://oss.arxitics.com/images/favicon.svg)