HR: 1330h
AN: SH42B-0536    [PDF]
TI: Turbulent Magnetic Field Generation in Rotating Stars
AU: * Bercik, D J
EM: bercik@ssl.berkeley.edu
AF: Space Sciences Laboratory, University of California 7 Gauss Way, Berkeley, CA 94720-7450 United States
AU: Abbett, W P
EM: abbett@ssl.berkeley.edu
AF: Space Sciences Laboratory, University of California 7 Gauss Way, Berkeley, CA 94720-7450 United States
AU: Fisher, G H
EM: fisher@ssl.berkeely.edu
AF: Space Sciences Laboratory, University of California 7 Gauss Way, Berkeley, CA 94720-7450 United States
AU: Fan, Y
EM: yfan@hao.ucar.edu
AF: High Altitude Observatory, National Center for Atmospheric Research 3450 Mitchell Lane, Boulder, CO 80301 United States
AB: Observationally, it has been found that magnetic activity is a strong function of rotation rate. The connection between rotation and dynamo-generated fields is not well understood, however. The typical interface dynamo theory applied to the Sun to describe its activity cycle assumes the existence of a velocity shear layer. Such a model is inappropriate for fully convective stars that are nevertheless active, such as late-type M and L stars and pre-main sequence T Tauri stars; in these stars a turbulent dynamo is generally believed to be the mechanism of magnetic field generation. We investigate the connection between observed activity behavior and magnetic field generation in fully convective stars through a series of simulations of the turbulent dynamo. The simulations were performed in a Cartesian domain using ANMHD, a 3D MHD anelastic code. We compare the resulting magnetic topologies for a series of Rossby numbers and comment on the implications for the sizes of coronal loops and activity levels.
UR: http://solarmuri.ssl.berkeley.edu/~fisher/public/images/turbdyn/
DE: 7500 SOLAR PHYSICS, ASTROPHYSICS, AND ASTRONOMY
DE: 7524 Magnetic fields
DE: 7539 Stellar astronomy
DE: 7544 Stellar interiors and dynamo theory
SC: SPA - Solar and Heliospheric Physics [SH]
MN: 2003 Fall Meeting