Simulations of Convection and Magnetism in Fully Convective Stars

Details Simulations of Convection and Magnetism in Fully Convective Stars Simulations of Convection and Magnetism in Fully Convective Stars

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...209.8908b&link_type=abstract

2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #89.08; Bulletin of the American Astronomical Society, V

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We present three-dimensional simulations of convection and magnetism within fully convective low-mass stars. Our spherical computational domain encompasses the bulk of the convective interior of a 0.3 solar mass M-dwarf, rotating at the solar angular velocity. We use the Anelastic Spherical Harmonic (ASH) code to examine highly nonlinear flows that extend over multiple scale heights and 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, the character of the convective flows, and the nature of the differential rotation established within the interior.

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