Numerical solution of the magnetostatic equations for thick flux tubes, with application to sunspots, pores, and related structures

Details Numerical solution of the magnetostatic equations for thick flux tubes, with application to sunspots, pores, and related structures Numerical solution of the magnetostatic equations for thick flux tubes, with application to sunspots, pores, and related structures

Mar 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...302..785p&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 302, March 15, 1986, p. 785-808.

Astronomy and Astrophysics

Astrophysics

82

Magnetohydrodynamics, Magnetostatics, Solar Magnetic Field, Sunspots, Boundary Value Problems, Field Strength, Iterative Solution, Magnetic Flux, Photosphere

Scientific paper

An iterative numerical technique permitting the solution, in great generality, of the nonlinear boundary value problem associated with two-dimensional magnetostatic equilibrium, and which may be extended to any geometry with one ignorable coordinate and to discontinuous configurations, is presently explored for two cases in the context of solar magnetic fields. A model sunspot is generated, and its structure and photometric signature are compared with previous models. It is demonstrated that the magnetic field configuration of vertically oriented flux tubes in the neighborhood of the solar furnace depends on (1) magnetic field strength, (2) the radius of the tube, (3), the net internal-external pressure deficit, and (4) the vertical dimensions of the pressure deficit layer. A scaling relation is derived to indicate when the magnetic topology will experience significant constriction in the Wilson (1977) depression.

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