Numerical simulation of spontaneous magnetic reconnection in solar atmosphere. (II). 2.5D results with gravity and heat conduction.

Details Numerical simulation of spontaneous magnetic reconnection in solar atmosphere. (II). 2.5D results with gravity and heat conduction. Numerical simulation of spontaneous magnetic reconnection in solar atmosphere. (II). 2.5D results with gravity and heat conduction.

Nov 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998acasn..39..381c&link_type=abstract

Acta Astron. Sin., Vol. 39, No. 4, p. 381 - 391

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Solar Atmosphere: Magnetohydrodynamics, Solar Atmosphere: Magnetic Reconnection, Solar Corona: Mass Ejection

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This paper studies the 2.5-dimensional magnetic reconnection caused by tearing instability after anomalous resistivity is introduced into the solar atmosphere with force-free magnetic field. Effects of isotropic heat conduction on magnetic reconnection and on the structure of the diffusion region have also been analyzed. The results and their applications to some solar phenomena, such as solar flares, coronal mass ejections and streamers, are discussed.

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