Numerical simulation of reconnection in an emerging magnetic flux region

Details Numerical simulation of reconnection in an emerging magnetic flux region Numerical simulation of reconnection in an emerging magnetic flux region

Sep 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984soph...94..315f&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 94, Sept. 1984, p. 315-340. Research supported by the Science and Engineering Research Coun

Statistics

Computation

83

Computational Astrophysics, Magnetic Field Configurations, Magnetic Flux, Solar Magnetic Field, Boundary Value Problems, Current Density, Hydrodynamic Equations, Magnetohydrodynamics, Shock Wave Propagation

Scientific paper

The resistive MHD equations are numerically solved in two dimensions for an initial-boundary-value problem which simulates reconnection between an emerging magnetic flux region and an overlying coronal magnetic field. The emerging region is modelled by a cylindrical flux tube with a poloidal magnetic field lying in the same plane as the external, coronal field. The plasma betas of the emerging and coronal regions are 1.0 and 0.1, respectively, and the magnetic Reynolds number for the system is 2×103. At the beginning of the simulation the tube starts to emerge through the base of the rectangular computational domain, and, when the tube is halfway into the computational domain, its position is held fixed so that no more flux of plasma enters through the base. Because the time-scale of the emergence is slower than the Alfvén time-scale, but faster than the reconnection time-scale, a region of closed loops forms at the base. These loops are gradually opened and reconnected with the overlying, external magnetic field as time proceeds.

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