Evolution of Solar Magnetic Arcades. I. Ideal MHD Evolution under Footpoint Shearing

Details Evolution of Solar Magnetic Arcades. I. Ideal MHD Evolution under Footpoint Shearing Evolution of Solar Magnetic Arcades. I. Ideal MHD Evolution under Footpoint Shearing

Nov 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996apj...472..360c&link_type=abstract

Astrophysical Journal v.472, p.360

Astronomy and Astrophysics

Astronomy

21

Magnetohydrodynamics: Mhd, Methods: Numerical, Sun: Magnetic Fields

Scientific paper

The ideal MHD evolution of a single magnetic arcade undergoing footpoint motions in a two- dimensional Cartesian geometry is investigated using numerical simulation. Also, force-free states of the same arcade are constructed with the use of a magnetofrictional method, which is formulated differently from those used in previous studies. In MHD simulations, no instability or nonequilibrium is found to the value of shear 100 times as large as the footpoint separation in the potential field. The evolutionary sequence is composed of three distinct phases. The first phase is characterized by the increase of the toroidal field strength and the second phase by a sort of self-similar expansion. In the third phase, the formation and growth of a central current layer are conspicuous. With increasing shear, the maximum current density increases, the width of the current layer decreases, and the feet of the current layer, which bifurcates above the bottom boundary, get closer to each other. The field lines in the current layer tend to thread the bottom boundary nearly horizontally for a large shear. From our results, it is inductively inferred that the magnetic arcade in a two-dimensional Cartesian geometry approaches an open field as the shear increases indefinitely.

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