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On the Theory of Rotating Magnetic Stars

Published online by Cambridge University Press:  12 April 2016

G. A. E. Wright
G. A. E. Wright*
Affiliation:
The University of Manchester, Manchester, England

Abstract

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All observations of magnetic stars necessarily yield information only about their surface features. We are ignorant of the nature of the fields in the interiors of such stars, and equally we cannot be sure of the non-existence of interior fields in stars which are superficially non-magnetic. In fact, if we assume the truth of the ‘fossil’ theory – that the magnetic flux of an Ap star is a relic of the flux initially present in the gas cloud from which the star condensed – then it is surprising that magnetic stars are not observed to be much more common, since magnetic fields appear to be ubiquitous in interstellar gas clouds. For those stars with strong surface convection zones, we might expect that a fossil field of low energy would be expelled by the turbulence and would possibly be trapped in the interior. However, the majority of early-type stars with radiative envelopes also do not exhibit any observable magnetic field.

Type
Part III / Stellar Rotation in Binaries, Clusters, and Special Objects. Statistics of Stellar Rotation
Information
International Astronomical Union Colloquium , Volume 4: Stellar Rotation , 1970 , pp. 264 - 268
Copyright
Copyright © Reidel 1970

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