A numerical simulation of magnetic reconnection and radiative cooling in line-tied current sheets

Details A numerical simulation of magnetic reconnection and radiative cooling in line-tied current sheets A numerical simulation of magnetic reconnection and radiative cooling in line-tied current sheets

Oct 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991soph..135..361f&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 135, Oct. 1991, p. 361-391.

Physics

54

Coronal Loops, Current Sheets, Magnetic Field Reconnection, Magnetohydrodynamic Stability, Radiative Heat Transfer, Solar Magnetic Field, Boundary Conditions, Computerized Simulation, Optical Thickness, Radiant Cooling, Tearing Modes (Plasmas)

Scientific paper

Radiative MHD equations are used for an optically thin plasma to carry out a numerical experiment related to the formation of 'postflare' loops. The numerical experiment starts with a current sheet that is in mechanical and thermal equilibrium but is unstable to both tearing-mode and thermal-condensation instabilities. The current sheet is line-tied at one end to a photospheric-like boundary and evolves asymmetrically. The effects of thermal conduction, resistivity variation, and gravity are ignored. In general, reconnection in the nonlinear stage of the tearing-mode instability can strongly affect the onset of condensations unless the radiative-cooling time scale is much smaller than the tearing-mode time scale. When the ambient plasma is less than 0.2, the reconnection enters a regime where the outflow from the reconnection region is supermagnetosonic with respect to the fast-mode wave speed. In the supermagnetosonic regime the most rapidly condensing regions occur downstream of a fast-mode shock that forms where the outflow impinges on closed loops attached to the photospheric-like boundary. A similar shock-induced condensation might occur during the formation of 'postflare' loops.

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