2014ApJ...794...15J

We report here an analysis of the physical stellar parameters of the giant star HD 185351 using Kepler short-cadence photometry, optical and near infrared interferometry from CHARA, and high-resolution spectroscopy. Asteroseismic oscillations detected in the Kepler short-cadence photometry combined with an effective temperature calculated from the interferometric angular diameter and bolometric flux yield a mean density ρ_{sstarf}= 0.0130±0.0003 ρ_☉ and surface gravity log g = 3.280±0.011. Combining the gravity and density we find R_{sstarf}= 5.35±0.20 R_☉and M_{sstarf}= 1.99±0.23 M_☉. The trigonometric parallax and CHARA angular diameter give a radius R_{sstarf}= 4.97±0.07 R_☉. This smaller radius, when combined with the mean stellar density, corresponds to a stellar mass 1.60±0.08 M_☉, which is smaller than the asteroseismic mass by 1.6σ. We find that a larger mass is supported by the observation of mixed modes in our high-precision photometry, the spacing of which is consistent only for M_{sstarf} ≳ 1.8 M_☉. Our various and independent mass measurements can be compared to the mass measured from interpolating the spectroscopic parameters onto stellar evolution models, which yields a model-based mass M_{sstarf}, model_= 1.87±0.07 M_☉. This mass agrees well with the asteroseismic value, but is 2.6σ higher than the mass from the combination of asteroseismology and interferometry. The discrepancy motivates future studies with a larger sample of giant stars. However, all of our mass measurements are consistent with HD 185351 having a mass in excess of 1.5 M_☉.