The Eclipsing Binary V1061 Cygni: Confronting Stellar Evolution Models for Active and Inactive Solar‐Type Stars
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Abstract
(Abridged) We present spectroscopic and photometric observations of the eclipsing system V1061 Cyg (P = 2.35 days). We show that it is a hierarchical triple in which the third star is visible in the spectra. We combine the radial velocities for the three stars, times of eclipse, and intermediate astrometric data from the HIPPARCOS mission (abscissa residuals) to establish the elements of the outer orbit (P = 15.8 yr) and accurate values for the masses and radii (1-2% errors) and the effective temperatures of the binary components. Both stars are rotating rapidly and have their rotation synchronized with the orbital motion. There are signs of activity including strong X-ray emission and possibly spots. Current stellar evolution models agree well with the properties of the primary, but show a very large discrepancy in the radius of the secondary: the predicted values are about 10% smaller than observed (a 5-sigma effect). Also, the temperature is cooler than predicted by some 200 K. These discrepancies are quite remarkable given that the star is only 7% less massive than the Sun, the calibration point of all stellar models. We identify the chromospheric activity as the likely cause of the effect. Inactive stars agree very well with the models, while active ones such as V1061 Cyg Ab appear systematically too large and too cool. Theory provides an understanding of this in terms of the strong magnetic fields commonly associated with stellar activity, which tend to inhibit convective heat transport.