Computer Science
Scientific paper
Nov 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984esasp.220..119m&link_type=abstract
In ESA The Hydromagnetics of the Sun p 119-122 (SEE N85-25091 14-92)
Computer Science
3
Computerized Simulation, Magnetic Field Configurations, Magnetohydrodynamics, Radiative Transfer, Solar Prominences, Stellar Models, Coronal Loops, Current Sheets, Tearing Modes (Plasmas)
Scientific paper
The radiative-resistive MHD equations are numerically solved in two dimensions for a magnetic field configuration that starts with a vertical current sheet which is line-tied at its base and is in mechanical, but not radiative, equilibrium. Whether this initial configuration can achieve a prominence-like equilibrium in the presence of magnetic reconnection and tearing in the current sheet is considered. Even though gravity was not incorporated into the system of equations, results indicate that the initial current sheet results in a Kuperus-Raady type of prominence and a Kippenhahn-Schluter type. The former occurs in the region above the X-line and is unstable, while the latter appears in the region below the X-line and is stable (i.e., the region of closed field line loops that develop at the base of the initial current sheet by reconnection). The effects of the radiative and nonradiative tearing modes upon the prominences are discussed.
Forbes Terry G.
Malherbe Jean-Marie
Priest Eric R.
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