Cool Stars 14 - Submitted Abstract # 191
This version created on 05 October 2006

Global Simulations of Convection and Magnetism in M-dwarfs


Matthew Browning, UC Berkeley
Gibor Basri, UC Berkeley

We present the results of three-dimensional simulations of convection
and magnetism within fully convective low-mass stars at varying
rotation rates.  Our spherical computational domain encompasses most
of the convective interior of a 0.3 solar mass M-dwarf.  We utilize
the Anelastic Spherical Harmonic (ASH) code, running on massively
parallel supercomputers, to examine highly nonlinear flows that can
admit magnetic dynamo action.  We find that small seed magnetic fields
are amplified by many orders of magnitude and sustained against Ohmic
decay.  We assess the strength and morphology of the resulting
magnetism, as well as the character of the convective and zonal flows
that are established within the interior.

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