Physics
Scientific paper
Aug 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998plth.conf..211h&link_type=abstract
Proceedings of the Second Asian Pacific Plasma Theory Conference (APPTC 1997), p. 211
Physics
High Temperature Plasmas, Plasma Temperature, Thermal Plasmas, Magnetic Field Reconnection, Magnetic Islands, Magnetohydrodynamic Stability, Magnetohydrodynamics, Plasmas (Physics), Solar X-Rays, Tearing Modes (Plasmas), Current Sheets, Electrical Resistivity, Parallel Computers, Solar Corona, Solar Flares, Solar Magnetic Field, Protostars, Simulation
Scientific paper
Recent X-ray astronomical observations show that magnetohydrodynamic (MHD) view is of vital importance in understanding the dynamics of the X-ray emitting hot plasmas in the universe. Especially they show that magnetic reconnection plays a key role. The Solar X-ray satellite, Yohkoh, showed various evidences of magnetic reconnection in solar corona. Here we extend the magnetic reconnection model of solar flares to hard X-ray flares observed in star forming regions. We carried out 2.5-dimensional magnetohydrodynamic (MHD) simulations of the disk-star interaction. The closed magnetic loops connecting the central star and the disk are twisted by the rotation of the disk. In the presence of resistivity, magnetic reconnection takes place in the current sheet formed inside the expanding loops. Hot, outgoing plasmoid and post flare loops are formed as a result of the reconnection. Numerical results are consistent with the observed plasma temperature (107 - 108)K, the length of the flaring loop (1011 - 1012)cm, and the velocity of optical jets (200 - 400km/s). We showed by high-resolution numerical simulations using parallel computers that multiple magnetic islands are created in the current sheet due to the growth of the tearing mode instability. The magnetic islands are ejected quasi-periodically. the intermittent flaring activity continues so long as the disk matter twists the post-flare loops.
Hayashi Mitsuru
Matsumoto Hyoji
Shibata Kazunari
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