Time-series Spectroscopy of the Oscillating Algol-type Binary AB Cas

Hong, Kyeongsoo; Lee, Jae Woo; Koo, Jae‐Rim; Lee, Chung-Uk; Park, Jang-Ho; Rittipruk, Pakakaew

doi:10.3847/1538-3881/aa6c25

Cited by 22 publications

(28 citation statements)

References 32 publications

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“…The process was very similar to that used by Hong et al (2017), and the search results are presented in Figure 3. We found the best-fitting parameters of T eff,1 = 8260 ± 210 K and v 1 sini = 72 ± 5 km s −1 .…”

Section: Observations and Data Analysismentioning

confidence: 83%

“…From eclipse-subtracted light residuals in both bands, they detected two frequencies of 41.87 cycle d −1 and 34.75 cycle d −1 and confirmed the δ Sct-like pulsation nature of the EB system. This article is the fourth contribution in a series of detailed studies, based on time-series spectroscopic observations of pulsating EBs (Hong et al 2015(Hong et al , 2017Koo et al 2016). Here, we present OO Dra as a pulsating post-mass transfer R CMa star evolving from a semi-detached Algol into an EL CVn-type binary, a new class of EBs defined by Maxted et al (2014a).…”

Section: Introductionmentioning

confidence: 99%

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

Lee

Hong

Koo

et al. 2017

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OO Dra is a short-period Algol system with a δ Sct-like pulsator. We obtained timeseries spectra between 2016 February and May to derive the fundamental parameters of the binary star and to study its evolutionary scenario. The radial velocity (RV) curves for both components were presented, and the effective temperature of the hotter and more massive primary was determined to be T eff,1 = 8260 ± 210 K by comparing the disentangling spectrum and the Kurucz models. Our RV measurements were solved with the BV light curves of Zhang et al. (2014) using the Wilson-Devinney binary code. The absolute dimensions of each component are determined as follows:Comparison with stellar evolution models indicated that the primary star resides inside the δ Sct instability strip on the main sequence, while the cool secondary component is noticeably overluminous and oversized. We demonstrated that OO Dra is an oscillating post-mass transfer R CMa-type binary; the originally more massive star became the low-mass secondary component through mass loss caused by stellar wind and mass transfer, and the gainer became the pulsating primary as the result of mass accretion. The R CMa stars, such as OO Dra, are thought to have formed by non-conservative binary evolution and ultimately to evolve into EL CVn stars.

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Section: Observations and Data Analysismentioning

confidence: 83%

Section: Introductionmentioning

confidence: 99%

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

Lee

Hong

Koo

et al. 2017

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“…With the FDBinary code (Ilijić et al 2004) 3 , we obtained a disentangling spectrum with a better SNR for the primary component and performed χ 2 minimization between the reconstructed and model spectra. This procedure is very similar to that employed by Hong et al (2017). For measuring the temperature (T eff,1 ) and the rotational velocity (v 1 sini), we chose eight absorption lines (Ca II K λ3933, H δ , Ca I λ4226, Fe I λ4271, H γ , Fe I λ4383, Mg II λ4481, and H β ).…”

Section: Spectral Analysismentioning

confidence: 99%

The Pre-He White Dwarfs in Eclipsing Binaries. I. WASP 0131+28

Lee,

Koo,

Hong

et al. 2020

Preprint

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We report the first BV light curves and high-resolution spectra of the post-mass transfer binary star WASP 0131+28 to study the absolute properties of extremely lowmass white dwarfs. From the observed spectra, the double-lined radial velocities were derived, and the effective temperature and rotational velocity of the brighter, more massive primary were found to be T eff,1 = 10, 000 ± 200 K and v 1 sini = 55 ± 10 km s −1 , respectively. The combined analysis of the TESS archive data and ours yielded the accurate fundamental parameters of the program target. The masses were derived to about 1.0 % accuracy and the radii to 0.6 %, or better. The secondary component's parameters of M 2 = 0.200 ± 0.002 M ⊙ , R 2 = 0.528 ± 0.003 R ⊙ , T eff,2 = 11,186 ± 235 K, and L 2 = 3.9 ± 0.3 L ⊙ are in excellent agreement with the evolutionary sequence for a helium-core white dwarf of mass 0.203 M ⊙ , and indicates that this star is halfway through the constant luminosity phase. The results presented in this article demonstrate that WASP 0131+28 is an EL CVn eclipsing binary in a thin disk, which is formed from the stable Roche-lobe overflow channel and composed of a main-sequence dwarf with a spectral type A0 and a pre-He white dwarf.

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“…Although a number of pulsating EBs have been found from various channels such as Kepler (Borucki et al 2010;) and the Transiting Exoplanet Survey Satellite (TESS; Ricker et al 2015), the samples for physical properties are still insufficient, so accurate study of these objects is required. Recently, a series of papers (Hong et al 2015(Hong et al , 2017(Hong et al , 2019Koo et al 2016;Lee et al 2018Lee et al , 2020 has contributed to studying the fundamental parameters of pulsating EBs.…”

Section: Introductionmentioning

confidence: 99%

Physical Nature of the Eclipsing δ Scuti Star AO Serpentis

Park,

Lee,

Hong

et al. 2020

Preprint

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We present the absolute properties of the eclipsing binary AO Ser with a pulsating component from our BV photometric and high-resolution spectroscopic observations, which were performed between April and May 2017. The radial velocities (RVs) for both components were measured, and the effective temperature and projected rotational velocity of the primary star were determined to be T eff,1 = 8,820 ± 62 K and v 1 sin i 1 = 90 ± 18 km s −1 , respectively, by comparing the observed spectrum with the Kurucz models. The accurate fundamental parameters of AO Ser were determined by a simultaneous analysis of the light and RV curves. The masses and radii of the primary and secondary components are M 1 = 2.55 ± 0.09 M ⊙ and R 1 = 1.64 ± 0.02 R ⊙ and M 2 = 0.49 ± 0.02 M ⊙ and R 2 = 1.38 ± 0.02 R ⊙ , respectively. Multiple frequency analyses for the eclipsesubtracted light residuals were conducted. As a result, we detected two frequencies of f 1 = 21.852 days −1 and f 2 = 23.484 days −1 . The evolutionary position on the HR diagram and the pulsational characteristics indicate that the primary star is a δ Sct pulsator with a radial fundamental mode. On the other hand, the relatively evolved secondary is oversized for its own mass.

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Time-series Spectroscopy of the Oscillating Algol-type Binary AB Cas

Cited by 22 publications

References 32 publications

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

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

The Pre-He White Dwarfs in Eclipsing Binaries. I. WASP 0131+28

Physical Nature of the Eclipsing δ Scuti Star AO Serpentis

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