Global-scale Magnetism (and Cycles) in Dynamo Simulations of Stellar Convection Zones

Type Conference Paper
Names B. P. Brown, M. K. Browning, A. S. Brun, M. S. Miesch, J. Toomre, Christopher M. Johns-Krull, Matthew K. Browning, Andrew A. West
Proceedings Title ASP Conference Series
Conference Name 16th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun. proceedings of a conference held August 28- September 2, 2010 at the University of Washington, Seattle, Washington.
Place San Francisco, CA
Publisher Astronomical Society of the Pacific
Volume 448
Pages 277
Series ASP Conference Series
Date December 1, 2011
Library Catalog NASA ADS
Abstract Young solar-type stars rotate rapidly and are very magnetically active. The magnetic fields at their surfaces likely originate in their convective envelopes where convection and rotation can drive strong dynamo action. Here we explore simulations of global-scale stellar convection in rapidly rotating suns using the 3-D MHD anelastic spherical harmonic (ASH) code. The magnetic fields built in these dynamos are organized on global-scales into wreath-like structures that span the convection zone. We explore one case rotates five times faster than the Sun in detail. This dynamo simulation, called case D5, has repeated quasi-cyclic reversals of global-scale polarity. We compare this case D5 to the broader family of simulations we have been able to explore and discuss how future simulations and observations can advance our understanding of stellar dynamos and magnetism.
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