| 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 |
| URL |
http://adsabs.harvard.edu/abs/2011ASPC..448..277B |
| 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. |