Variability of quiescent and flaring radio emission in RS CVn and Algol-type binary systems

Details Variability of quiescent and flaring radio emission in RS CVn and Algol-type binary systems Variability of quiescent and flaring radio emission in RS CVn and Algol-type binary systems

Mar 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...283..483l&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 283, no. 2, p. 483-492

Statistics

Computation

17

Binary Stars, Computational Astrophysics, Flare Stars, Radio Astronomy, Radio Emission, Stellar Activity, Stellar Evolution, Stellar Luminosity, Electron Flux Density, Light Curve, Stellar Coronas, Stellar Flares, Synchrotron Radiation, Time Series Analysis, Very Large Array (Vla)

Scientific paper

The temporal evolution of the 5 GHz emission of RS CVn and Algol type binaries is studied. About 70 hours of very large array (VLA) observations of six systems are used. It is shown that the emission is time variable both during flares and during a significant fraction of the 'quiescent' phases, on time scales ranging from tens of minutes to some hours. The observed time scales are qualitatively discussed with respect to several possible processes. The directivity of optically thin and thick gyrosynchrotron emission might account for the recurrent phase-dependent behaviour. Variations shorter than approximately 1 h are probably related to the evolution of the radiating electrons. The occultation of radio sources with substellar size might, however, act on similar time scales and must not be ignored even if definite evidence for such features does not exist. The comparison between the observed short time scales of variation and the expected life times suggests that the permanent radio emission of these binary systems is due to the continuous or repetitive energization of electrons is these stellar coronae during and outside large flares.

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