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Detection of a sub-milliarcsecond radio component in the RS CVn system HR 1099
Lestrade, J. F.; Mutel, R. L.; Phillips, R. B.; Webber, J. C.; Niell, A. E.; Preston, R. A.
AA(Iowa, University, Iowa City, IA), AB(Haystack Observatory, Westford, MA), AC(Haystack Observatory, Westford, MA), AD(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AE(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA)
Astrophysical Journal, Part 2 - Letters to the Editor (ISSN 0004-637X), vol. 282, July 1, 1984, p. L23-L26. Research sponsored by the University of Iowa and Groupe de Recherche de Geodesie Spatiale. (ApJL Homepage)
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NASA/STI Keywords:
Binary Stars, Radio Stars, Stellar Radiation, Variable Stars, Brightness Temperature, Chromosphere, K Stars, Very Long Base Interferometry
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The RS CVn system HR 1099 was observed with a five station VLBI array at a frequency of 8.4 GHz during a strong radio outburst of approximately 400 mJy. The data are consistent with a circular Gaussian source of 0.8 + or - 0.12 milli-arcsec (FWHM), corresponding to a linear size of 4 + or - 0.6 x 10 to the 11th cm. This is comparable to the distance between the surfaces of the two stars, or to 75 percent of the diameter of the chromospherically active K star. Extrapolation of published photometric data shows that the starspot formation of HR 1099 was facing toward the observers at the times of observations. The high equivalent brightness temperature, approximately 10 billion K, is consistent with gyrosynchrotron emission from a power-law energy distribution of electrons in a magnetic field of strength about 30 gauss.

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