Asteroseismic inference on rotation, gyrochronology and planetary system dynamics of 16 Cygni. Issue 3 (29th November 2014)

• Record Type: Journal Article
• Authors: Davies, G. R.; Chaplin, W. J.; Farr, W. M.; García, R. A.; Lund, M. N.; Mathis, S.; Metcalfe, T. S.; Appourchaux, T.; Basu, S.; Benomar, O.; Campante, T. L.; Ceillier, T.; Elsworth, Y.; Handberg, R.; Salabert, D.; Stello, D.
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 446:Issue 3(2015)
• Page Start: 2959
• Page End: 2966
• Publication Date: 2014-11-29
• Subjects: planet–star interactions -- stars: oscillations -- stars: rotation; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stu2331
• Languages: English
• ISSNs: 0035-8711

Abstract

Abstract: The solar analogues 16 Cyg A and 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 $23.8^{+1.5}_{-1.8}$ and $23.2^{+11.5}_{-3.2} \rm \, d$, and the angles of inclination to be $56^{+6}_{-5} \, ^{\circ }$ and $36^{+17}_{-7} \, ^{\circ }$, 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.