VLBI imaging of the RS CVn binary star system HR 5110

Details VLBI imaging of the RS CVn binary star system HR 5110 VLBI imaging of the RS CVn binary star system HR 5110

2003-01-21

arxiv.org/abs/astro-ph/0301413v1

Astrophys.J. 587 (2003) 390-397

Astronomy and Astrophysics

Astrophysics

22 pages, 4 figures

Scientific paper

10.1086/368070

We present VLBI images of the RS CVn binary star HR 5110 (=BH CVn; HD 118216), obtained from observations made at 8.4 GHz on 1994 May 29/30 in support of the NASA/Stanford Gravity Probe B project. Our images show an emission region with a core-halo morphology. The core was 0.39 +/- 0.09 mas (FWHM) in size, or 66% +/- 20% of the 0.6 +/- 0.1 mas diameter of the chromospherically active K subgiant star in the binary system. The halo was 1.95 +/- 0.22 mas (FWHM) in size, or 1.8 +/- 0.2 times the 1.1 +/- 0.1 mas separation of the centers of the K and F stars. The core increased significantly in brightness over the course of the observations and seems to have been the site of flare activity that generated an increase in the total flux density of ~200% in 12 hours. The fractional circular polarization simultaneously decreased from ~10% to 2.5%.

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