The evolution of line-tied coronal arcades including a converging footpoint motion

Details The evolution of line-tied coronal arcades including a converging footpoint motion The evolution of line-tied coronal arcades including a converging footpoint motion

Apr 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992soph..138..257i&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 138, no. 2, April 1992, p. 257-281. Research supported by DOE and NASA.

Physics

69

Magnetic Energy Storage, Magnetohydrodynamics, Solar Corona, Solar Magnetic Field, Solar X-Rays, Solar Flares, Solar Prominences, Solar Temperature, Time Dependence

Scientific paper

It has been demonstrated in the past that single, 2D coronal arcades are very unlikely driven unstable by a simple shear of the photospheric footpoints of the magnetic field lines. By means of 2D, time-dependent MHD simulations, evidence is presented that a resistive instability can result if in addition to the footpoint shear a slow motion of the footpoints toward the photospheric neutral line is included. The photospheric footpoint velocity in this model is nonsingular and the shear dominates everywhere. Starting from a planar potential field geometry for the arcade, it is found that after some time a current sheet is formed which is unstable with respect to the tearing instability. The time of its onset scales with the logarithm of the magnetic diffusivity assumed in the calculation. In its nonlinear phase, a quasi-stationary situation arises in the vicinity of the x-line with an almost constant reconnection rate. The height of the x-line above the photosphere and the distance of the separatrix footpoints remain almost constant in this phase, while the helical flux tube, formed above the neutral line, continuously grows in size.

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