Magnetic reconnection in coronal loops

Details Magnetic reconnection in coronal loops Magnetic reconnection in coronal loops

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sh41a07g&link_type=abstract

American Geophysical Union, Spring Meeting 2001, abstract #SH41A-07

Physics

7509 Corona, 7835 Magnetic Reconnection, 7843 Numerical Simulation Studies

Scientific paper

Magnetic reconnection corresponds to a change in the connectivity of magnetic fieldlines and to the transfer of magnetic energy to the plasma. Therefore, it must play an important role in the heating of active regions of the solar corona. We study reconnection processes in elongated coronal loops driven at their footpoints by convective motions. The reduced magnetohydrodynamic (RMHD) approximation is appropriate in systems displaying a strong magnetic field in their axial direction and much smaller transverse components, and whose gradients are larger in the transverse directions. We present numerical simulations of the RMHD equations, which show the reconnection of two flux tubes being twisted from the boundaries by a stationary velocity pattern consisting of two vortices rotating in the same direction. Relevant global quantities such as the reconnection rate and the energy dissipation rate are computed for different forcing intensities. The dynamics of the velocity and magnetic fields is also studied, and different reconnection regimes are identified.

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