The equilibrium structure of thin magnetic flux tubes. II

Details The equilibrium structure of thin magnetic flux tubes. II The equilibrium structure of thin magnetic flux tubes. II

May 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...304..519k&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 304, May 1, 1986, p. 519-525. Research supported by the Harvard-Smithsonian

Astronomy and Astrophysics

Astrophysics

14

Atmospheric Temperature, Magnetic Flux, Magnetohydrodynamics, Radiative Transfer, Solar Magnetic Field, Stellar Magnetic Fields, Equilibrium Equations, Late Stars, Light Curve, Sun

Scientific paper

The thermal structure of the medium inside thin, vertical magnetic flux tubes embedded in a given external atmosphere is investigated, assuming cylindrical symmetry and a depth-independent plasma beta. The variation with tube radius of the temperature on the tube axis is computed and the temperature on the tube wall is estimated. The temperature variation across the flux tube is found to be due to the depth variation of the intensity and to the density stratification of the atmosphere. Since the temperature difference between the axis and the wall is small in thin flux tubes (of the order of 10 percent), the horizontal temperature gradient may often be neglected and the temperature in a tube of given radius may be described by a single function of depth. Thus, a more detailed numerical treatment of the radiative transfer within thin flux tubes can be substantially simplified by neglecting horizontal temperature differences within the flux tube proper.

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