Astronomy and Astrophysics – Astronomy
Scientific paper
Aug 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998apj...502l.177t&link_type=abstract
Astrophysical Journal Letters v.502, p.L177
Astronomy and Astrophysics
Astronomy
77
Convection, Magnetohydrodynamics: Mhd, Sun: Interior, Sun: Magnetic Fields, Galaxy: Globular Clusters: General
Scientific paper
A plausible scenario for solar dynamo action is that the large-scale organized toroidal magnetic field is generated by the action of strong radial shear at the base of the solar convection zone, whereas the weaker poloidal field is regenerated by cyclonic convection throughout the convection zone. We show, using high-resolution three-dimensional numerical simulations, that the required transport of magnetic field from the convection zone to the overshoot region can be achieved on a convective rather than diffusive timescale by a pumping mechanism in turbulent penetrative compressible convection. A layer of magnetic field initially placed in the convection zone is swept down by strong sinking plumes, locally amplified, and deposited in the stable region at the base of the convection zone, despite the opposing action of magnetic buoyancy. The rate of transport is insensitive to the strength of the initial imposed field.
Brummell Nicholas H.
Clune Thomas L.
Tobias Steven M.
Toomre Juri
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