S. J. Murphy, A. Pigulski, D. W. Kurtz, J.-C. Suárez, G. Handler, L. A. Balona, B. Smalley, K. Uytterhoeven, R. Szabó, A. O. Thygesen, V. G. Elkin, M. Breger, A. Grigahcène, J. A. Guzik, J. M. Nemec, J. Southworth
Abstract
The candidate SX Phe star KIC 11754974 shows a remarkably high number of combination frequencies in the Fourier amplitude spectrum: 123 of the 166 frequencies in our multi-frequency fit are linear combinations of independent modes. Predictable patterns in frequency spacings are seen in the Fourier transform of the light curve. We present an analysis of 180 d of short-cadence Kepler photometry and of new spectroscopic data for this evolved, late A-type star. We infer from the1150-d, long-cadence light curve, and in two different ways, that our target is the primary of a 343-d, non-eclipsing binary system. According to both methods, the mass function is similar, ƒ(M) = 0.0207 ± 0.0003M☉. The observed pulsations are modelled extensively, using separate, state-of-the-art, time-dependent convection (TDC) and rotating models. The models match the observed temperature and low metallicity, finding a mass of 1.50–1.56M☉. The models suggest the whole star is metal-poor, and that the low metallicity is not just a surface abundance peculiarity. This is the best frequency analysis of an SX Phe star, and the only Kepler δ Sct star to be modelled with both TDC and rotating models.
Keywords
asteroseismology - stars: individual: KIC 11754974 - Stars: oscillations - stars: Population II - stars: variables: δ Scuti
Notes
There's an erratum for this paper available here.
Monthly Notices of the Royal Astronomical Society
Volume 432, Issue 3, Page 2284
2013 July
