Abstract
The strongest magnetic fields on the sun are those of sunspots. Although their magnetic fields have been studied for a long time much remains unknown about the magnetism of these principal sources. At sufficiently large distances from a spot the magnetic field can, apparently, be well approximated as that of a dipole submerged below the solar photosphere, (classical Mt. Wilson observations of Hale, 1919; Bumba, 1960; Severny, 1964). However, a more detailed study of the distribution of magnetic fields inside the spot shows the fine structure of the field. The field is concentrated in bundles, small elements, showing twisting and vorticities, somewhere inside a sunspot (Severny, 1964; Stepanov and Gopasyuk, 1962). The field is also appreciably inhomogeneous, and has fine structure shown by a local maximum of the field strength at a certain depth (Guseeynov, 1969), the strong rotation of the transverse component of the magnetic field with depth (Severny, 1964), the fine structure in the pattern of vertical electric currents (Severny, 1964; Kotov, 1970).
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Severny, A.B. (1972). Local Magnetic Fields on the Sun. In: de Jager, C., Dyer, E.R. (eds) Solar-Terrestrial Physics/1970. Astrophysics and Space Science Library, vol 29. Springer, Dordrecht. https://doi.org/10.1007/978-94-010-3126-4_4
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DOI: https://doi.org/10.1007/978-94-010-3126-4_4
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