Core Convection and Dynamo Action in Rotating A-type Stars

Details Core Convection and Dynamo Action in Rotating A-type Stars Core Convection and Dynamo Action in Rotating A-type Stars

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aas...205.3403b&link_type=abstract

American Astronomical Society Meeting 205, #34.03; Bulletin of the American Astronomical Society, Vol. 36, p.1402

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We have carried out 3-D simulations of core convection and dynamo activity within A-type stars of two solar masses at a range of rotation rates. Our models consider the inner 30% by radius of such stars, thus capturing the entire convective core and a portion of the surrounding radiative envelope within the spherical computational domain. Using the anelastic spherical harmonic (ASH) code on massively parallel supercomputers, we solve the compressible MHD equations to examine highly nonlinear and evolving flows and magnetic fields. Vigorous dynamo action is realized, with initial seed magnetic fields amplified by many orders of magnitude and sustained against ohmic decay. The resulting complex magnetism possesses energy densities comparable to that in the flows, is structured on many scales, and serves to modify the convective and zonal flows that gave rise to it. The differential rotation established in progenitor hydrodynamic simulations is weakened, and waxes and wanes in strength as the simulations evolve. We discuss the morphology and evolution of the flows and magnetic fields, the penetrative properties of the convection, and the nature of the dynamo process.

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