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The Boundary between the Magnetic Fields of Ap Stars and the Fields of Solar-type Stars

Published online by Cambridge University Press:  12 April 2016

John D. Landstreet
John D. Landstreet*
Affiliation:
Department of Astronomy, The University of Western Ontario London, Ontario N6A 3K7, Canada

Abstract

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The boundary between Ap-type magnetic fields and the magnetic fields of solar-type stars occurs near Te ~ 7000K, about where deep envelope convection develops in main sequence stars. This seems natural for solar-type stars, in which the field is generated by the convection zone. However, among magnetic Ap stars the frequency of occurrence declines from about 10% of all A stars near A0 to about 1% near F0. It is not clear what produces this decline in frequency, but the convection zone is probably not responsible. In fact, it seems likely that if global fossil fields occur in main sequence F stars, such fields should be detectable even if the stars having them are not chemically peculiar.

Type
Part IV Stellar activity
Information
International Astronomical Union Colloquium , Volume 130: The Sun and Cool Stars: activity, magnetism, dynamos , 1991 , pp. 342 - 346
Copyright
Copyright © Springer-Verlag 1991

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