Dec 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993nyu..rept.....s&link_type=abstract
Annual Report, 1 Jan. - 31 Dec. 1993 New York Univ., New York, NY. Inst. of Mathematical Sciences.
Mathematics
Ballooning Modes, Magnetic Field Reconnection, Magnetohydrodynamic Stability, Magnetohydrodynamics, Solar Flares, Boundary Conditions, Computerized Simulation, Magnetic Fields, Solar Corona, Two Dimensional Models
Scientific paper
During the past year, several topics were studied which are important for solar MHD. These include: (1) 3D coalescence instability and magnetic reconnection. Magnetic reconnection is fairly well understood in two dimensional theory and numerical simulations in which there is an ignorable coordinate. It is poorly understood in three dimensional line tied magnetic fields, which are the generic case in solar flux loops. The 3D line tied coalescence MHD instability was investigated both analytically and numerically. In the nonlinear stages of the simulation, the instability drives magnetic reconnection. As in earlier 3D forced reconnection simulations, an intense current layer forms where magnetic energy is converted to heat. It was found that while line tying somewhat inhibits reconnection, it does not prevent it; (2) Line tied gravitational ballooning instability. A new two dimensional prominence model was found and its stability was analyzed. This instability might describe the irregular rain falling from prominences. Boundary conditions for the solar corona. It has been the practice to model the effects of the chromosphere and photosphere only through their influence on the boundary conditions imposed at the base of the corona.
Hameiri Eliezer
Strauss Harald
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