A numerical simulation of two-dimensional radiative equilibrium in magnetostatic flux tubes. I - The model

Details A numerical simulation of two-dimensional radiative equilibrium in magnetostatic flux tubes. I - The model A numerical simulation of two-dimensional radiative equilibrium in magnetostatic flux tubes. I - The model

Feb 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...404..788p&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 404, no. 2, p. 788-798.

Astronomy and Astrophysics

Astrophysics

15

Magnetohydrostatics, Solar Atmosphere, Solar Magnetic Field, Stellar Models, Radiative Transfer, Sunspots

Scientific paper

We describe an efficient numerical procedure for obtaining self-consistent radiative and mechanical equilibria of solar magnetostatic flux tubes. The flux tube is treated as a localized but continuous concentration of magnetic flux in a two-dimensional slab geometry. Starting from some given initial atmosphere, we compute a preliminary magnetostatic equilibrium state by a nonlinear iterative technique, subject to certain boundary conditions on the magnetic field. Given the resulting spatial distribution of opacities (derived from the initial run of temperature and density along each field line), and with knowledge of a distant radiation field incident upon the magnetic region, the radiative state of the atmosphere is computed by the short-characteristics method assuming gray, LTE conditions. The new temperature derived from the angle-averaged radiation field is used to update the hydrostatic atmosphere for the magnetostatic calculation, and so on, until both mechanical and radiative balance is attained.

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