Absolute Properties of the Pulsating Post-mass Transfer Eclipsing Binary OO Draconis

Lee, Jae Woo; Hong, Kyeongsoo; Koo, Jae‐Rim; Park, Jang-Ho

doi:10.3847/1538-3881/aa947e

Cited by 27 publications

(13 citation statements)

References 46 publications

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“…Thus, we adjusted the rotation parameter of F 1 = v 1,rot / v 1,sync = 0.68 in the binary modeling, and the resulting binary solutions are coincident with those of F 1 = 1.0 within their uncertainties. As in the case of OO Dra (Lee et al 2018) and V404 Lyr (Lee et al 2020), the parameter of rotation rate F indicated a weak sensitivity in this binary solution.…”

Section: Binary Modeling and Absolute Dimensionssupporting

confidence: 55%

BD+47 378: An Eclipsing Binary Containing a δ Sct Pulsating Star

Hong¹,

Lee²,

Rittipruk³

et al. 2022

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New high-resolution spectra of the eclipsing binary BD+47 378 were obtained on five nights between 2020 and 2021 with the Bohyunsan Observatory Echelle Spectrograph in Korea. We collected the TESS light curve of the system obtained from Sectors 17 to 18, which shows a flat bottom at the secondary eclipse, an O’Connell effect, and oscillation features. From the spectral analysis, the radial velocities (RVs) of the primary and secondary stars were obtained, and the temperature of the brighter and more massive primary component was determined to be 7140 ± 100 K. According to a simultaneous analysis of the double-lined RVs and TESS light curves, the masses and radii of both components are M 1 = 1.69 ± 0.03 M ⊙, M 2 = 0.80 ± 0.02 M ⊙, R 1 = 2.01 ± 0.01 R ⊙, and R 2 = 0.79 ± 0.01 R ⊙, respectively. The primary component of the system is located on the δ Sct and γ Dor instability strips. After subtracting the theoretical light curve from the TESS data, a total of four independent frequencies (5.7235 day−1, 6.2577 day−1, 6.9588 day−1, and 14.7675 day−1) were detected using the multiple frequency analysis. These frequencies are typical of a δ Sct pulsator. The results reveal that BD+47 378 is a detached system consisting of two main-sequence stars with a δ Sct type primary component.

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Section: Binary Modeling and Absolute Dimensionssupporting

confidence: 55%

BD+47 378: An Eclipsing Binary Containing a δ Sct Pulsating Star

Hong¹,

Lee²,

Rittipruk³

et al. 2022

Self Cite

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“…Struve (1946) reported that his results were not fully exempted from rotational broadening and line blending between the components. Trailed spectra are of great use in revealing and tracking the orbital motions of binary stars (e.g., Lee et al 2018Lee et al , 2020aLee et al , 2020b. In order to look for sets of absorption lines for X Tri, we made the phase-folded trailed spectra from the BOES observations and examined them in detail at full wavelength.…”

Section: New Spectroscopy and Data Analysismentioning

confidence: 99%

Absolute Properties of the Oscillating Eclipsing Algol X Trianguli

Lee

Hong

Park

et al. 2023

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We report results from the TESS photometric data and new high-resolution spectra of the Algol system X Tri showing short-period pulsations. From the echelle spectra, the radial velocities of the eclipsing pair were measured, and the rotational rate and effective temperature of the primary star were obtained to be v 1sini = 84 ± 6 km s−1 and T eff,1 = 7900 ± 110 K, respectively. The synthetic modeling of these observations implies that X Tri is in synchronous rotation and is physically linked to a visual companion TIC 28391715 at a separation of about 6.″5. The absolute parameters of our target star were accurately and directly determined to be M 1 = 2.137 ± 0.018 M ⊙, M 2 = 1.101 ± 0.010 M ⊙, R 1 = 1.664 ± 0.010 R ⊙, R 2 = 1.972 ± 0.010 R ⊙, L 1 = 9.67 ± 0.55 L ⊙, and L 2 = 2.16 ± 0.09 L ⊙. The phase-binned mean light curve was used to remove the binary effect from the observed TESS data. Multifrequency analysis of the residuals revealed 16 significant frequencies, of which the high-frequency signals between 37 day−1 and 48 day−1 can be considered probable pulsation modes. Their oscillation periods of 0.021−0.027 days and pulsation constants of 0.014−0.018 days are typical values of δ Sct variables. The overall results demonstrate that X Tri is an oEA star system consisting of a δ Sct primary and its lobe-filling companion in the semidetached configuration.

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“…To validate the ICC approach, this study revisits two wellknown objects, δ Sct-type pulsating primary stars in the doublelined eclipsing binary systems AB Cas 1 and OO Dra. These two δ Sct primaries differ from classical δ Sct stars in evolutionary terms due to mass transfer between the binary components (Hong et al 2017;Lee et al 2018;Mkrtichian et al 2022); their binary evolution is described in Section 5.2. They have an important advantage from an asteroseismic aspect in that their physical properties, such as masses and radii, are well constrained from photometric and spectroscopic observations.…”

Section: Introductionmentioning

confidence: 99%

Asteroseismic Determination of Stellar Rotation: On Synchronization in the Close Eclipsing Binaries AB Cas and OO Dra

Kim

2023

ApJ

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A star’s rotation rate is difficult to estimate without surface inhomogeneities such as dark or bright spots. This paper presents asteroseismic results to determine the rotation rates of δ Sct-type pulsating primary stars in two eclipsing binary systems, AB Cas and OO Dra. After removing the binarity-induced light variations from archival TESS data and carefully examining the combination frequencies, we identified 12 independent frequencies for AB Cas and 11 frequencies for OO Dra, with amplitudes higher than ∼0.3 mmag, as δ Sct-type pulsation frequencies excited in each primary star. The theoretical frequencies for seismic analysis were obtained by fully considering rotation effects. Grid fitting for various stellar properties, such as mass, radius, metallicity, and rotation rate, yielded the best solutions for which the theoretical frequencies and stellar parameters agreed well with the observations. The rotation rate of the AB Cas primary was tightly constrained to 0.81 ± 0.01 day−1 (f rot/f orb = 1.11 − 0.02 + 0.01 ), which is slightly faster than the synchronized rotation. In contrast, the rotation rate of 0.63 ± 0.01 day−1 for the OO Dra primary is lower than the synchronous value of approximately 0.81 day−1. Subsynchronous rotation is uncommon in short-period binaries, and its physical mechanism is not yet well understood. Our results show that asteroseismology can be used to measure the rotation rate of fast-rotating δ Sct stars precisely and thus provide a valuable constraint on rotation–orbit synchronization in close binary systems.

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Absolute Properties of the Pulsating Post-mass Transfer Eclipsing Binary OO Draconis

Cited by 27 publications

References 46 publications

BD+47 378: An Eclipsing Binary Containing a δ Sct Pulsating Star

BD+47 378: An Eclipsing Binary Containing a δ Sct Pulsating Star

Absolute Properties of the Oscillating Eclipsing Algol X Trianguli

Asteroseismic Determination of Stellar Rotation: On Synchronization in the Close Eclipsing Binaries AB Cas and OO Dra

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