摘要：We present the first high-resolution spectra for the eclipsing binary V404 Lyr showing γ Dor pulsations, which we use to study its absolute properties.By fitting models to the disentangling spectrum of the primary star, we found that it has an effective temperature of Teff,1 = 7330 ± 150 K and a rotational velocity of v1 sin i = 148 ± 18 km s−1.The simultaneous analysis of our double-lined radial velocities and the pulsation-subtracted Kepler data gives us accurate stellar and system parameters of V404 Lyr.The masses, radii, and luminosities are M1 = 2.17 ± 0.06 M⊙, R1 = 1.91 ± 0.02 R⊙, and L1 = 9.4 ± 0.8 L⊙ for the primary, and M2 = 1.42 ± 0.04 M⊙, R2 = 1.79 ± 0.02 R⊙, and L2 = 2.9 ± 0.2 L⊙ for the secondary.The tertiary component orbiting the eclipsing pair has a mass of M3b = 0.71 ± 0.15 M⊙ in an orbit of P3b = 642 ± 3 days, e3b = 0.21 ± 0.04, and a3b = 509 ± 2 R⊙.The third light of l3 = 4.1% ± 0.2% could be partly attributable to the K-type circumbinary object.By applying a multiple frequency analysis to the eclipse-subtracted light residuals, we detected 45 frequencies with signal-to-noise amplitude ratios larger than 4.0.Identified as independent pulsation modes, seven frequencies (f1 − f6, f9), their new pulsation constants, and the location in the Hertzsprung–Russell diagram indicate that the pulsating primary is a γ Dor-type variable star.
关键词：Eclipsing binary stars;Fundamental parameters of stars;Stellar oscillations;Spectroscopy;Multi-periodic pulsation;Asteroseismology
