Very long baseline interferometry observations of the RS Canum Venaticorum system HR 5110 at 8.4 GHz

Details Very long baseline interferometry observations of the RS Canum Venaticorum system HR 5110 at 8.4 GHz Very long baseline interferometry observations of the RS Canum Venaticorum system HR 5110 at 8.4 GHz

Apr 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...279..184l&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 279, April 1, 1984, p. 184-187. Research supported by the Centre National d

Astronomy and Astrophysics

Astronomy

22

Binary Stars, Radio Astronomy, Stellar Radiation, Very Long Base Interferometry, Brightness Temperature, Radiant Flux Density, Stellar Magnitude

Scientific paper

The RS CVn binary system HR 5110 was observed with a well-calibrated four-element VLBI array at a frequency of 8.4 GHz. The total flux density, which was nearly constant at 32 + or - 2 mJy, was monitored throughout the experiment with a 20 km baseline interferometer allowing accurate visibilities to be calculated. The observed visibilities are consistent with a source unresolved on all the baselines. The maximum size of the equivalent Gaussian source is 1.4 milli-arcsec (FWHM), corresponding to a linear size of 1.1 x 10 to the 12th cm at 52 pc. This maximum size is comparable with the overall size of the binary system. The inferred lower limit of the brightness temperature is 4 x 10 to the 8th K, which is higher than the coronal temperature of 10 to the 7th K measured in a soft X-ray survey. This is consistent with a nonthermal mechanism for the radiation process of the moderate radio outburst observed.

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