Computer Science
Scientific paper
Feb 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003esasp.517..201b&link_type=abstract
In: Proceedings of SOHO 12 / GONG+ 2002. Local and global helioseismology: the present and future, 27 October - 1 November 2002,
Computer Science
12
Convection, Magnetic Fields
Scientific paper
We report on results from a series of radiative magnetoconvection simulations in a 12 Mm×12 Mm×3 Mm near-surface solar layer. Initially unipolar, vertical magnetic field at average field strengths of 0 G, 200 G and 400 G is imposed on a fully relaxed hydrodynamic convective state. Magnetic field is swept to the intergranular boundaries by the convective flows, where it is compressed to kilogauss field strenghts. The shapes and intensities of magnetic features typically evolve on the same time scale as the granulation pattern; however, the underlying magnetic structure evolves on a much longer time scale. Occasionally, dark, high field strength features form that have properties consistent with observed micropores. The micropores primarily form when a small granule submerges and the surrounding magnetic field moves into the resulting dark "hole". The fluid flow inside micropores is suppressed by the strong magnetic field. The surrounding walls of a micropore experiences a net cooling through vertical radiation. The resulting thermodynamic structure of micropores stabilize them against destruction, allowing some micropores to exist for many granulation time scales.
Bercik David John
Nordlund Aake
Stein Robert F.
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