Solar Flare MDH
Annual rept. 1 Jan-31 Dec 1993
NEW YORK UNIV NY COURANT INST OF MATHEMATICAL SCIENCES
Pagination or Media Count:
During the past year, several topics were studied which are important for solar MHD. These include 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. 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.
- Electricity and Magnetism
- Plasma Physics and Magnetohydrodynamics