Force-free fields in thin coronal loops

Details Force-free fields in thin coronal loops Force-free fields in thin coronal loops

Aug 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...431..873e&link_type=abstract

The Astrophysical Journal, vol. 431, no. 2, pt. 1, p. 873-880

Astronomy and Astrophysics

Astrophysics

1

Coronal Loops, Force-Free Magnetic Fields, Magnetic Flux, Magnetohydrodynamics, Plasma Pressure, Solar Magnetic Field, Cosmology, Mathematical Models, Plasma Compression, Toroidal Plasmas

Scientific paper

We solve the force-free equation J x B = 0 for fields which are toroidally symmetric. The technique utilizes an expansion about a cylindrical field and is therefore valid or tori with a large aspect ratio such as long, thin, coronal loops. The calculation is performed in spatial toroidal coordinates, rather than in the flux coordinates used by previous authors; this allows direct calculation of the loci of flux surfaces and of surfaces of constant magnetic pressure. Our solutions differ significantly from toroidal fields in laboratories, which are in general not force-free. They are characterized by field lines whose projections in the poloidal planes are circles with centers displaced by varying distances from the axis of the torus. In general, flux surfaces do not correspond to surfaces of constant magnetic pressure. We have examined solutions corresponding to simple analytic zero-order cylindrical fields. For moderate twists in the zero-order (cylindrical) field, the magnetic pressure is larger on the inner toroidal radius. However, this effect diminishes with twist angle and in fact, for extreme initial twists, the magnetic pressure can be larger on the outer radius. We compare our results with previous work utilizing flux coordinates.

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