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Properties of Stellar Magnetic Fields in Close Binaries Deduced from Non-Thermal Radio Observations

Published online by Cambridge University Press:  30 March 2016

R. L. Mutel
R. L. Mutel*
Affiliation:
Department of Physics and Astronomy University of IowaIowa City, IA 52242USA

Abstract

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Analysis of VLA and VLBI observations of non-thermal radio emission from close binary stellar systems can produce reliable estimates of magnetic field strength and geometry in the source emission region. Assuming a gyrosynchrotron emission model for the non-flare emission, one can model the magnetic field as a relatively small number of stable magnetic loops of overall size R ⋍ (1-3)×1012 cm. with an average field strength of 101 < B < 102 gauss. A correlation of mean fractional circular polarization with inclination angle along with an absence of any clear phase dependence, indicates that the loops are azimuthally symmetric with poles nearly orthogonal to the orbital plane, i.e. axisymmetric dipolar. The loops are probably the same as the loops derived from observations of x-ray emission of ‘hot’ (T ⋍ 107K) coronal gas.

Type
Joint Discussions
Information
Highlights of Astronomy , Volume 7: Highlights of Astronomy. As presented at the XIXth General Assembly of the IAU, 1985 , 1986 , pp. 457 - 460
Copyright
Copyright © Reidel 1986

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