On the magnetic and thermodynamic consequences of the return-flux sunspot model

Details On the magnetic and thermodynamic consequences of the return-flux sunspot model On the magnetic and thermodynamic consequences of the return-flux sunspot model

Oct 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...261..700f&link_type=abstract

Astrophysical Journal, Part 1, vol. 261, Oct. 15, 1982, p. 700-709.

Astronomy and Astrophysics

Astrophysics

33

Magnetic Flux, Magnetohydrostatics, Solar Magnetic Field, Sunspots, Nonlinear Equations, Penumbras, Photosphere, Pressure Distribution, Solar Corona, Temperature Distribution, Umbras

Scientific paper

The magnetic structure of sunspots from photosphere to low corona is considered on the basis of a new magnetohydrostatic theory of sunspots. The first numerical solutions of the basic nonlinear force-balance equation which takes into account returning magnetic flux are obtained using observational data for the maximum field, umbral, and penumbral size and for the vertical distribution of pressure on the sunspot axis and in the quiet sun. Both vertical and horizontal distributions for the magnetic field were obtained as well as its vertical gradient. Further, the pressure and temperature distributions consistent with this field were also obtained. The dependence of the model on the Wilson depression, the maximum magnetic field of the sunspot, and the amount of return magnetic flux is investigated. A 'global' force-balance relation is found to hold which relates the magnetic field gradient on the spot axis with the maximum magnetic field and the pressure deficit, or Wilson depression, in the spot photosphere.

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