Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...436..907f&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 436, no. 2, p. 907-928
Astronomy and Astrophysics
Astronomy
133
Magnetic Flux, Magnetohydrodynamic Flow, Solar Activity, Solar Convection (Astronomy), Solar Magnetic Field, Solar Rotation, Stellar Models, Toroidal Plasmas, Computerized Simulation, Mathematical Models
Scientific paper
The buoyant rise of a magnetic flux loop arising from a single perturbed segment of a toroidal flux ring lying slightly beneath the base of the convection zone is studied by way of numerical simulations. We have considered flux loop evolution assuming both solid-body rotation, and differential rotation consistent with recent results from helioseismology. Our major results are presented, and we offer some speculations on the decay of active regions, based on the results of our studies. We speculate that as plasma in the tube attempts to establish hydrostatic equilibrium along the field lines after the flux emergence has taken place, the tube field strength at some intermediate depths below the surface becomes sufficiently small at the surface portions of the tube (which have cooled and undergone convective collapse) become dynamically disconnected from those portions near the base of the convection zone. The surface proportions of the emerged flux tubes are then transported by motions near the photosphere, such as supergranular convection and meridional flow.
Fan Ying
Fisher George H.
McClymont Alexander N.
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