Line-tied magnetic reconnection

Details Line-tied magnetic reconnection Line-tied magnetic reconnection

Sep 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987soph..114..311r&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 114, no. 2, 1987, p. 311-327. SERC-supported research.

Physics

6

Magnetic Field Configurations, Magnetic Field Reconnection, Solar Flares, Boundary Conditions, Boundary Layer Flow, Computerized Simulation, Current Sheets, Plasma Turbulence, Tearing Modes (Plasmas)

Scientific paper

Two-dimensional numerical simulations of magnetic reconnection in a configuration relevant to two-ribbon solar flares are presented. The calculations extend those of Forbes and Priest (1982, 1983) and some puzzling aspects of their results are clarified. In particular, the roles of magnetic diffusion, of the tearing mode, and of turbulence are individually examined. The important part played by boundary conditions in determining the evolution of the initial current sheet is stressed, and it is suggested that in the future the evolution of the entire overlying magnetic arcade be modeled as well as the current sheet that is created below the rising arcade. Tearing at very high magnetic Reynolds numbers is likely to develop into an impulsive bursty regime of reconnection after a time which depends on the initial level of turbulence.

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