Asteroseismic inference on rotation, gyrochronology and planetary system dynamics of 16 Cygni

Abstract

The solar analogs 16 Cyg A and 16 Cyg B are excellent asteroseismic targets in the \Kepler field of view and together with a red dwarf and a Jovian planet form an interesting system. For these more evolved Sun-like stars we cannot detect surface rotation with the current \Kepler data but instead use the technique of asteroseimology to determine rotational properties of both 16 Cyg A and B. We find the rotation periods to be $23.8_{-1.8}^{+1.5}\mathrm{days}$ and $23.2_{-3.2}^{+11.5}\mathrm{days}$, and the angles of inclination to be $56_{-5}^{+6}{}^{\circ }$ and $36_{-7}^{+17}{}^{\circ }$, for A and B respectively. Together with these results we use the published mass and age to suggest that, under the assumption of a solar-like rotation profile, 16 Cyg A could be used when calibrating gyrochronology relations. In addition, we discuss the known 16 Cyg B star-planet eccentricity and measured low obliquity which is consistent with Kozai cycling and tidal theory.

10 pages accepted for publication in the MNRAS

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