Absolute Properties of the Eclipsing γ Dor Star V404 Lyrae

Abstract

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 T eff,1 = 7, 330 ± 150 K and a rotational velocity of v 1 sini = 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 M 1 = 2.17±0.06 M ⊙ , R 1 = 1.91±0.02 R ⊙ , and L 1 = 9.4±0.8 L ⊙ for the primary, and M 2 = 1.42±0.04 M ⊙ , R 2 = 1.79±0.02 R ⊙ , and L 2 = 2.9±0.2 L ⊙ for the secondary. The tertiary component orbiting the eclipsing pair has a mass of M 3b = 0.71±0.15 M ⊙ in an orbit of P 3b = 642±3 days, e 3b = 0.21±0.04, and a 3b = 509±2 R ⊙ . The third light of l 3 = 4.1 ± 0.2% could be partly attributable to the K-type circumbinary object. By applying a multiple frequency analysis to the eclipsesubtracted light residuals, we detected 45 frequencies with signal to noise amplitude ratios larger than 4.0. Identified as independent pulsation modes, seven frequencies (f 1 − f 6 , f 9 ), their new pulsation constants, and the location in the Hertzsprung-Russell diagram indicate that the pulsating primary is a γ Dor-type variable star.

The effect of tides on near-core rotation: analysis of 35 Kepler γ Doradus stars in eclipsing and spectroscopic binaries

“…1 shows the result of the eclipses removal, using KIC 3228863 as an example. The binary system and its third component were studied using the Kepler photometry and ground-based spectroscopy by Lee et al (2019). Our calculated period is 0.73094425 ± 0.00000004 d, consistent with their measurement.…”

“…The known γ Dor binaries whose period spacings were not previously measured are: KIC 3228863 (Lee et al 2019(Lee et al , 2014; KIC 4150611 (Hełminiak et al 2017); KIC 6048106 (Lee 2016;Samadi Ghadim, Lampens & Jassur 2018); KIC 6206751 (Lee & Park 2018); KIC 8569819 (Kurtz et al 2015); KIC 9236858 (Kjurkchieva & Atanasova 2016); and KIC 9851944 (Guo et al 2016). These works focused mainly on the dynamics of the binary systems, hence they did not measure the period spacings of g modes.…”

“…Lee et al (2019); (b) Lee et al (2014); (c) Li et al (2019b); (d) Li et al (2020); (e) Guo et al (2019); (f) Hełminiak et al (2017); (g) Kjurkchieva, Vasileva & Atanasova (2017); (h) Lee (2016); (i) Samadi Ghadim et al (2018); (j) Lee & Park (2018); (k) Guo & Li (2019); (l)Özdarcan & Dal (2017); (m) Li et al (2019a); (n) Sowicka et al (2017); (o) Kurtz et al (2015); (p) Kjurkchieva & Atanasova (2016); (q) Zhang et al (2020); (r) Guo et al (2017); (s) Guo et al (2016); (t) Keen et al (2015); (u) Schmid & Aerts (2016); (v) Schmid et al (2015); (w) Zhang et al (2018).…”

TESS Photometry of the Eclipsing $δ$ Scuti Star AI Hydrae

“…To develop this subject, we have been looking for pulsating stars in EBs and studying their physical properties, utilizing Kepler satellite photometry and ground-based spectroscopy (e.g., Lee & Park 2018;Lee et al 2020). Recently, the 2-min cadence observations of the Transiting Exoplanet Survey Satellite (TESS; Ricker et al 2015) have proved very helpful for asteroseismology of the pulsating EBs showing multiperiodic oscillation with low amplitudes (Lee et al 2019;Antoci et al 2019).…”

“…Lee et al 2020). The model parameters for the observed TESS data are given as Model 1 in columns (2)−(3) of Table3.…”