Abstract
Known potential field solutions can be used to model the structure of magnetic fields in the solar photosphere. Several two-dimensional and axisymmetric solutions are compared. In the most satisfactory model the vertical component of the field is prescribed on a horizontal plane so as to be uniform within a finite disc and zero outside it. The resulting flux distribution provides a good description of small scale intergranular magnetic fields and of the observed field structure in a pore, but is inadequate for sunspots.
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Simon, G.W., Weiss, N.O. & Nye, A.H. Simple models for magnetic flux tubes. Sol Phys 87, 65–75 (1983). https://doi.org/10.1007/BF00151161
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DOI: https://doi.org/10.1007/BF00151161