Other
Scientific paper
Sep 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...433..361k&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 433, no. 1, p. 361-378
Other
19
Magnetic Field Reconnection, Magnetic Relaxation, Magnetohydrodynamics, Solar Corona, Solar Flares, Solar Magnetic Field, Stellar Models, Computerized Simulation, Magnetic Field Configurations, Mathematical Models, Photosphere, Three Dimensional Models
Scientific paper
The magnetohydrodynamic (MHD) relaxation process in the solar coronal magnetic field is investigated in detail by using a three-dimensional MHD numerical simulation. The interaction between the magnetic loops which are located periodically above the photosphere is mainly considered. It is found that when each foot of the loops is twisted by the photospheric motion the loops aligned along the magnetic inversion line are reconnected with each other. The magnetic reconnection process successively proceeds, and as a result a large-scale magnetic field parallel to the inversion line is spontaneously generated. The process is an MHD relaxation process where the magnetic configuration evolves toward a linear force-free field predicted by Taylor and Heyvaerts & Priest. The Taylor-Heyvaerts-Priest hypothesis about the selective dissipation of the energy compared to the magnetic helicity is numerically verified. It is observed that a magnetic dip, which is a favorable environment for the prominence condensation, is spontaneously generated through the relaxation process. Finally, the solar flare as a relaxation process of the magnetic energy is discussed, based on the simulation results.
Kubo Harunobu
Kusano Kanya
Miyoshi Takahiro
Nishikawa Ken
Suzuki Yasuhiro
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