Computer Science
Scientific paper
Oct 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002esasp.505..385d&link_type=abstract
In: SOLMAG 2002. Proceedings of the Magnetic Coupling of the Solar Atmosphere Euroconference and IAU Colloquium 188, 11 - 15 Jun
Computer Science
Active Regions, Solar Magnetoconvection
Scientific paper
Vigorous fluid motions associated with the observed patterns of supergranulation, mesogranulation, and granulation are likely to play a large role during the evolution of magnetic field within solar active regions. To investigate such dynamics, we have constructed numerical simulations of fully compressible, magnetized fluids, each contained within curved, spherical segments that approximate conditions near the top of the solar convection zone. We present recent results of one three-dimensional simulation of an idealized bipolar active region contained within a thin spherical segment. The segment nominally spans 30° in latitude and 60° in longitude, and has a radial extent of 4% of the solar radius. Upon initialization, the domain is threaded by a bipolar radial magnetic field, which subsequently cancels as the ensuing convection advects field horizontally across the segment. We find that the time scale at which the field decays is slower than the expected turbulent decay time scale, and is much closer to the diffusive (Ohmic) decay time scale, despite the network of convection cells surrounding the magnetized regions. We suggest that this convection serves to confine field of like polarity and thus suppresses the turbulent decay of magnetic field.
Alexander Dave
de Rosa Marc L.
Hurlburt Neal E.
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