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Radio Emission from Starspots on RSCVn Binary HR1099

Published online by Cambridge University Press:  25 April 2016

John D. Bunton ,
R. T. Stewart ,
O. B. Slee ,
G. J. Nelson ,
Alan E. Wright ,
Julian B. Corbin ,
David R. Brown  and
P. J. Hall
John D. Bunton
Affiliation:
Department of Electrical Engineering, University of Sydney
R. T. Stewart
Affiliation:
Division of Radiophysics, CSIRO, Sydney
O. B. Slee
Affiliation:
Division of Radiophysics, CSIRO, Sydney
G. J. Nelson
Affiliation:
Division of Radiophysics, CSIRO, Sydney
Alan E. Wright
Affiliation:
Division of Radiophysics, CSIRO, Sydney
Julian B. Corbin
Affiliation:
Department of Electrical Engineering, University of Sydney
David R. Brown
Affiliation:
Department of Electrical Engineering, University of Sydney
P. J. Hall
Affiliation:
Division of Radiophysics, CSIRO, Sydney
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Abstract

Properties of the microwave emission from HR1099 are examined in an attempt to determine whether the emission arises as gyro-synchrotron radiation from mildly relativistic electrons trapped in magnetic fields above starspots on the active K subgiant component. It is shown that radio curves do not exhibit a systematic variation in phase with the rotation rate, as one might expect for emission from a source situated above a long-lived starspot. However, there is some evidence that the radio flaring occurs at two preferred longitude zones. Whether these zones agree with starspot locations remains to be determined by light curve modelling. What we can say with confidence is that the measured spectral index of the microwave emission does not fit a simple gyro-synchrotron source model, such as that proposed to explain the observed reversal with frequency of the sense of circular polarization.

Type
Contributions
Information
Publications of the Astronomical Society of Australia , Volume 6 , Issue 3 , 1986 , pp. 316 - 319
Copyright
Copyright © Astronomical Society of Australia 1986

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