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Quiescent Non-thermal Radio Emission from Stellar Systems

Published online by Cambridge University Press:  25 April 2016

Michelle C. Storey  and
R. G. Hewitt
Michelle C. Storey
Affiliation:
Research Centre for Theoretical Astrophysics, School of Physics, University of Sydney, NSW 2006, Australia. michelle@physics.usyd.edu.au
R. G. Hewitt
Affiliation:
Department of Theoretical Physics, School of Physics, University of Sydney, NSW 2006, Australia
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Abstract

Non-thermal radio emission has been detected from dMe stars, RS CVn binaries and W T Tauri stars. Polarisation and intensity measurements of the quiescent (i.e. non-flaring) emission indicate that the emission is gyrosynchrotron emission from mildly relativistic electrons spiralling in a magnetic field. A three-dimensional dipole magnetic field model for the stellar field is presented and the quiescent gyrosynchrotron emission from such a model is calculated and compared with observations. The model can account for many phenomenological features of quiescent emission. Quantitative comparisons of model results with observations indicate that the electron distribution in the emission region may be a magnetic mirroring distribution.

Keywords

starsflare — radiation mechanismscyclotron and synchrotron — radiative transfer
Type
Galactic and Stellar
Information
Publications of the Astronomical Society of Australia , Volume 12 , Issue 2 , August 1995 , pp. 174 - 179
Copyright
Copyright © Astronomical Society of Australia 1995

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