Statistics – Computation
Scientific paper
Dec 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...21110309b&link_type=abstract
American Astronomical Society, AAS Meeting #211, #103.09; Bulletin of the American Astronomical Society, Vol. 39, p.920
Statistics
Computation
Scientific paper
I analyze the effects of varying rotation rate in nonlinear 3-D MHD simulations of fully convective M-dwarfs. The spherical computational domain in these simulations encompasses most of the convective interior of a 0.3 solar-mass M-dwarf. Using the anelastic spherical harmonic code ASH,
I examine the convective flows, differential rotation, and dynamo action achieved in the interiors of such stars, focusing here on how the flows and magnetic fields respond to variations in the overall frame rotation rate. I find that under weak rotational constraints, differential rotation is established in hydrodynamic simulations and may persist in the presence of modest dynamo-generated magnetic fields. As the rotation rate increases, the level of sustained magnetic energy realized by the dynamo grows; for a narrow range of field strengths, intricate feedbacks between the differential rotation and magnetic energy can be realized. When rotation is still more rapid, magnetic fields in excess of equipartition are attained, and act essentially to eliminate the differential rotation. Because the convective flows in these low-mass stars are very slow, rotation is strong relative to inertia even for solar-like rotation rates, suggesting that differential rotation should be rare in M-stars with measurable rotational velocities. Even in the absence of differential rotation, the dynamo-generated magnetic fields possess structure on a variety of spatial scales, including a prominent axisymmetric mean component.
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