Magnetic Fields in Stellar Bodies: II. Magnetic Fields in Upper Main Sequence Stars

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Abstract
Following the analysis given in an earlier paper the structure of a weak, poloidal magnetic field inside a non-rotating, upper main sequence star has been calculated for the case where the external field is dipole-like. The non-linear equations involved have been solved using a successive approximation technique which is rapidly convergent. The calculations show that the field structure is similar to that deduced for compressible polytropes in that the current associated with the field has an approximate radial variation proportional to the product of density and radius. It therefore has a sharp maximum deep inside the star.

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