Other
Scientific paper
May 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21640802y&link_type=abstract
American Astronomical Society, AAS Meeting #216, #408.02; Bulletin of the American Astronomical Society, Vol. 41, p.815
Other
Scientific paper
The magnetic reconnection is one of the fundamental processes for the heating, bulk flow acceleration, and magnetic topology change in the solar/stellar atmospheres and other astrophysical energetic phenomena. For the quantitative understanding of these phenomena, it is crucially important to determine the energy release rate or, equivalently, the reconnection rate from numerical studies. Owing to the enormously large magnetic Reynolds number, it is expected that the MHD turbulence or some stochastic process may play a role for the magnetic diffusion in the reconnection region. By performing three-dimensional MHD simulations, we are working on this issue. The temporal evolution of a simple current sheet with initially imposed fluctuations in the resistivity is studied. A substantial increase of energy release ratewas found by adding the guide field, i.e. the field parallelto the electric current. It is interpreted that this is due to the mutual interactions of magnetic islands formed in a spatially separated parallel resonant layers.
Isobe Hiroaki
Yokoyama Takaaki
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