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  • Park, Jang-Ho  (12)
  • 1
    Online Resource
    Online Resource
    Time-series Spectroscopy of the Oscillating Eclipsing Algol System V392 Orionis
    American Astronomical Society ; 2019
    In:  The Astronomical Journal Vol. 157, No. 1 ( 2019-01-01), p. 28-
    Details
    In: The Astronomical Journal, American Astronomical Society, Vol. 157, No. 1 ( 2019-01-01), p. 28-
    Abstract: We present the results from a detailed analysis of our high-resolution spectra and historical photometric observations of the semidetached eclipsing binary V392 Ori with a δ Scuti ( δ Sct) pulsating component. A total of 31 spectroscopic observations were carried out at both the Bohyunsan Optical Astronomy Observatory in Korea and the Thai National Observatory in Thailand during the 2016 and 2017 observing seasons. The radial velocities (RVs) of the primary and the faint secondary components were determined, and the effective temperature and projected rotational velocity of the former star were measured as T eff,1  = 8500 ± 160 K and v 1 sin i  = 148 ± 13 km s −1 , respectively, through a comparison of the observed spectra and stellar atmosphere models. The physical properties of V392 Ori were determined by analysis of our RVs together with the existing multiband light curves. The results are the following: masses of M 1  = 2.28 ± 0.30 M ⊙ and M 2  = 0.49 ± 0.10 M ⊙ , and radii of R 1  = 2.08 ± 0.09 R ⊙ and R 2  = 1.15 ± 0.05 R ⊙ . The primary star located inside the main-sequence band exhibits a δ Sct-type pulsation. On the contrary, the less massive secondary component is significantly oversized and overluminous for its mass and temperature.
    Type of Medium: Online Resource
    ISSN: 0004-6256 , 1538-3881
    URL: Article
    DOI: 10.3847/1538-3881/aaf39f
    RVK:
    US 1090
    Language: Unknown
    Publisher: American Astronomical Society
    Publication Date: 2019
    detail.hit.zdb_id: 127191-X
    detail.hit.zdb_id: 2003104-X
    SSG: 16,12
    Location Call Number Limitation Availability
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  • 2
    Online Resource
    Online Resource
    Absolute Dimensions and Apsidal Motions of Three Binary Systems in the Large Magellanic Cloud
    American Astronomical Society ; 2019
    In:  The Astronomical Journal Vol. 158, No. 5 ( 2019-11-01), p. 185-
    Details
    In: The Astronomical Journal, American Astronomical Society, Vol. 158, No. 5 ( 2019-11-01), p. 185-
    Abstract: We present the physical properties and apsidal motion elements of three eccentric eclipsing binaries in the Large Magellanic Cloud. The time-series photometric observations were carried out for a total of 41 nights between 2018 November and 2019 February using the KMTNet 1.6 m telescopes installed in South Africa and Australia. The radial velocities of binary components were measured using about 15 spectra per system collected from the ESO Science Archive Facility, which were observed with the Very Large Telescope 8.2 m telescope. The effective temperatures of the more massive binary components were determined to be 19000 ± 500 K for OGLE-LMC-ECL-05797, 17000 ± 500 K for OGLE-LMC-ECL-05861, and 19000 ± 500 K for OGLE-LMC-ECL-06510 by comparing the observed spectra and the stellar atmosphere models obtained from the BOSZ spectral library. The absolute dimensions of each system were derived by analyzing the radial velocity curves together with the light curves obtained from the KMTNet, OGLE, and MACHO observations during about three decades. For the apsidal motion study, new eclipse timings were derived from the KMTNet and survey photometry. The apsidal motion elements of the three binaries were determined from both light curve and eclipse timing analysis. The periods of apsidal motion were 67 ± 2 yr for OGLE-LMC-ECL-05797, 124 ± 6 yr for OGLE-LMC-ECL-05861, and 39 ± 1 yr for OGLE-LMC-ECL-06510 and their internal structure constants (ISCs) were log , and −2.1 ± 0.1 in the same order. The observed ISCs of OGLE-LMC-ECL-05797 and OGLE-LMC-ECL-05861 showed a good match to the theoretical ISC values, while the value of OGLE-LMC-ECL-06510 was somewhat larger than the theoretical one.
    Type of Medium: Online Resource
    ISSN: 0004-6256 , 1538-3881
    URL: Article
    DOI: 10.3847/1538-3881/ab44ad
    RVK:
    US 1090
    Language: Unknown
    Publisher: American Astronomical Society
    Publication Date: 2019
    detail.hit.zdb_id: 127191-X
    detail.hit.zdb_id: 2003104-X
    SSG: 16,12
    Location Call Number Limitation Availability
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  • 3
    Online Resource
    Online Resource
    Absolute Properties of the Pulsating Post-mass Transfer Eclipsing Binary OO Draconis
    American Astronomical Society ; 2018
    In:  The Astronomical Journal Vol. 155, No. 1 ( 2018-01-01), p. 5-
    Details
    In: The Astronomical Journal, American Astronomical Society, Vol. 155, No. 1 ( 2018-01-01), p. 5-
    Abstract: OO Dra is a short-period Algol system with a δ Sct-like pulsator. We obtained time-series 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 K by comparing the disentangling spectrum and the Kurucz models. Our RV measurements were solved with the BV light curves of Zhang et al. using the Wilson-Devinney binary code. The absolute dimensions of each component are determined as follows: M 1  = 2.03 ± 0.06 , M 2  = 0.19 ± 0.01 , R 1  = 2.08 ± 0.03 , R 2  = 1.20 ± 0.02 , L 1  = 18 ± 2 , and L 2  = 2.0 ± 0.2 . 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.
    Type of Medium: Online Resource
    ISSN: 0004-6256 , 1538-3881
    URL: Article
    DOI: 10.3847/1538-3881/aa947e
    RVK:
    US 1090
    Language: Unknown
    Publisher: American Astronomical Society
    Publication Date: 2018
    detail.hit.zdb_id: 127191-X
    detail.hit.zdb_id: 2003104-X
    SSG: 16,12
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  • 4
    Online Resource
    Online Resource
    Absolute Dimensions and Evolutionary Status of the Semi-detached Algol W Ursae Minoris
    American Astronomical Society ; 2018
    In:  The Astronomical Journal Vol. 155, No. 3 ( 2018-03-01), p. 133-
    Details
    In: The Astronomical Journal, American Astronomical Society, Vol. 155, No. 3 ( 2018-03-01), p. 133-
    Abstract: Double-lined eclipsing binaries allow accurate and direct determination of fundamental parameters such as mass and radius for each component, and they provide important constraints on the stellar structure and evolution models. In this study, we aim to determine a unique set of binary parameters for the Algol system W UMi and to examine its evolutionary status. New high-resolution time-series spectroscopic observations were carried out during 14 nights from 2008 April to 2011 March, and a total of 37 spectra were obtained using the Bohyunsan Optical Echelle Spectrograph. We measured the radial velocities (RVs) for both components, and the effective temperature of the primary star was found to be T eff,1  = 9310 ± 90 K by a comparison of the observed spectra and the Kurucz models. The physical parameters of W UMi were derived by an analysis of our RV data together with the multi-band light curves of Devinney et al. The individual masses, radii, and luminosities of both components are M 1  = 3.68 ± 0.10 M ⊙ and M 2  = 1.47 ± 0.04 M ⊙ , R 1  = 3.88 ± 0.03 R ⊙ and R 2  = 3.13 ± 0.03 R ⊙ , and L 1  = 102 ± 1 L ⊙ and L 2  = 7.3 ± 0.1 L ⊙ , respectively. A comparison of these parameters with theoretical stellar models showed that the primary component lies in the main-sequence band, while the less massive secondary is noticeably evolved. The results indicate that the initially more massive star became the present secondary by losing most of its own mass via mass transfer to the companion (present primary).
    Type of Medium: Online Resource
    ISSN: 0004-6256 , 1538-3881
    URL: Article
    DOI: 10.3847/1538-3881/aaab65
    RVK:
    US 1090
    Language: Unknown
    Publisher: American Astronomical Society
    Publication Date: 2018
    detail.hit.zdb_id: 127191-X
    detail.hit.zdb_id: 2003104-X
    SSG: 16,12
    Location Call Number Limitation Availability
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  • 5
    Online Resource
    Online Resource
    Absolute Properties of the Eclipsing γ Dor Star V404 Lyrae
    American Astronomical Society ; 2020
    In:  The Astronomical Journal Vol. 159, No. 1 ( 2020-01-01), p. 24-
    Details
    In: The Astronomical Journal, American Astronomical Society, Vol. 159, No. 1 ( 2020-01-01), p. 24-
    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  = 7330 ± 150 K and a rotational velocity of v 1 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 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 3 b  = 0.71 ± 0.15 M ⊙ in an orbit of P 3 b  = 642 ± 3 days, e 3 b  = 0.21 ± 0.04, and a 3 b  = 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 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 ( 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.
    Type of Medium: Online Resource
    ISSN: 0004-6256 , 1538-3881
    URL: Article
    DOI: 10.3847/1538-3881/ab59ce
    RVK:
    US 1090
    Language: Unknown
    Publisher: American Astronomical Society
    Publication Date: 2020
    detail.hit.zdb_id: 127191-X
    detail.hit.zdb_id: 2003104-X
    SSG: 16,12
    Location Call Number Limitation Availability
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  • 6
    Online Resource
    Online Resource
    The Pre-He White Dwarfs in Eclipsing Binaries. I. WASP 0131+28
    American Astronomical Society ; 2020
    In:  The Astronomical Journal Vol. 160, No. 1 ( 2020-07-01), p. 49-
    Details
    In: The Astronomical Journal, American Astronomical Society, Vol. 160, No. 1 ( 2020-07-01), p. 49-
    Abstract: 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 low-mass 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 K and  = 55 ± 10 km s −1 , respectively. The combined analysis of the Transiting Exoplanet Survey Satellite (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 , ,  = 11,186 ± 235 K, and are in excellent agreement with the evolutionary sequence for a helium-core white dwarf of mass 0.203 , 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.
    Type of Medium: Online Resource
    ISSN: 0004-6256 , 1538-3881
    URL: Article
    DOI: 10.3847/1538-3881/ab9621
    RVK:
    US 1090
    Language: Unknown
    Publisher: American Astronomical Society
    Publication Date: 2020
    detail.hit.zdb_id: 127191-X
    detail.hit.zdb_id: 2003104-X
    SSG: 16,12
    Location Call Number Limitation Availability
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  • 7
    Online Resource
    Online Resource
    Photometric Properties of the HW Vir-type Binary OGLE-GD-ECL-11388
    IOP Publishing ; 2017
    In:  Publications of the Astronomical Society of the Pacific Vol. 129, No. 971 ( 2017-01-01), p. 014202-
    Details
    In: Publications of the Astronomical Society of the Pacific, IOP Publishing, Vol. 129, No. 971 ( 2017-01-01), p. 014202-
    Type of Medium: Online Resource
    ISSN: 0004-6280 , 1538-3873
    URL: Article
    DOI: 10.1088/1538-3873/129/971/014202
    Language: Unknown
    Publisher: IOP Publishing
    Publication Date: 2017
    detail.hit.zdb_id: 300625-6
    SSG: 16,12
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  • 8
    Online Resource
    Online Resource
    The Pre-He White Dwarfs in Eclipsing Binaries. II. WASP 0843–11
    American Astronomical Society ; 2021
    In:  The Astronomical Journal Vol. 161, No. 3 ( 2021-03-01), p. 137-
    Details
    In: The Astronomical Journal, American Astronomical Society, Vol. 161, No. 3 ( 2021-03-01), p. 137-
    Abstract: We present the Transiting Exoplanet Survey Satellite (TESS) photometry and our high-resolution spectra of the EL CVn–type star 1SWASP J084356.46–113327.5 (WASP 0843–11), which consists of an F-type main-sequence (MS) star and a hotter low-mass helium white dwarf precursor (pre-He WD). In a spectral analysis, double-lined radial velocities (RVs) were obtained for the first time. From a simultaneous analysis of the TESS light and RV curves, the masses, radii, and temperatures of each component were determined to be M 1 = 1.733 ± 0.031 M ⊙ , M 2 = 0.220 ± 0.008 M ⊙ , R 1 = 2.094 ± 0.013 R ⊙ , R 2 = 0.331 ± 0.003 R ⊙ , T 1 = 6960 ± 120 K, and T 2 =9870 ± 310 K, respectively. According to their physical properties, the primary and secondary stars are located on the instability strips of δ Sct/ γ Dor hybrids and extremely low-mass WDs, respectively. We applied multiple frequency analyses to the residual light curve after subtracting the binarity effects and detected a total of four independent frequencies. A frequency of f 3 = 1.6356 day −1 in the low-frequency region was reminiscent of γ Dor stars, while the other three frequencies of f 2 , f 15 , and f 18 in the high-frequency region (150–196 day −1 ) are probably related to pre-He WD components. Our results demonstrate that the more massive MS primary star of WASP 0843–11 is a γ Dor pulsator, whereas the hotter secondary component is a pre-He WD with high-frequency pulsations.
    Type of Medium: Online Resource
    ISSN: 0004-6256 , 1538-3881
    URL: Article
    DOI: 10.3847/1538-3881/abdd39
    RVK:
    US 1090
    Language: Unknown
    Publisher: American Astronomical Society
    Publication Date: 2021
    detail.hit.zdb_id: 127191-X
    detail.hit.zdb_id: 2003104-X
    SSG: 16,12
    Location Call Number Limitation Availability
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  • 9
    Online Resource
    Online Resource
    Time-series Spectroscopy of the Oscillating Algol-type Binary AB Cas
    American Astronomical Society ; 2017
    In:  The Astronomical Journal Vol. 153, No. 6 ( 2017-06-01), p. 247-
    Details
    In: The Astronomical Journal, American Astronomical Society, Vol. 153, No. 6 ( 2017-06-01), p. 247-
    Abstract: This study presents the high-resolution spectra of the eclipsing binary AB Cas with a δ Sct-type pulsating component, which were obtained using the Bohyunsan Optical Echelle Spectrograph in Korea. In this paper, the radial velocities for the primary and secondary stars were measured from a total of 27 spectra made during two nights in 2015 October. We derived accurate physical properties of the system for the first time by simultaneously analyzing our radial velocity curves together with previously published uvby light curves. Individual masses, radii, and effective temperatures of both components were determined to be M ⊙ and M ⊙ , R ⊙ and R ⊙ , and K and K, respectively. The results should be more accurate than previous photometric studies. We investigated the evolutionary history of AB Cas by comparing its physical parameters with stellar evolutionary models. The primary component is not a classical δ Sct pulsator but is the result of mass accretion transferred from the initial more massive star, which is the present secondary. This indicates that AB Cas is an oscillating Algol-type eclipsing binary with a low-mass and oversized secondary component filling its inner Roche lobe.
    Type of Medium: Online Resource
    ISSN: 0004-6256 , 1538-3881
    URL: Article
    DOI: 10.3847/1538-3881/aa6c25
    RVK:
    US 1090
    Language: Unknown
    Publisher: American Astronomical Society
    Publication Date: 2017
    detail.hit.zdb_id: 127191-X
    detail.hit.zdb_id: 2003104-X
    SSG: 16,12
    Location Call Number Limitation Availability
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  • 10
    Online Resource
    Online Resource
    Physical Nature of the Eclipsing δ Scuti Star AO Serpentis
    American Astronomical Society ; 2020
    In:  The Astronomical Journal Vol. 160, No. 6 ( 2020-12-01), p. 247-
    Details
    In: The Astronomical Journal, American Astronomical Society, Vol. 160, No. 6 ( 2020-12-01), p. 247-
    Abstract: 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 2017 April and May. 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  = 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 eclipse-subtracted 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.
    Type of Medium: Online Resource
    ISSN: 0004-6256 , 1538-3881
    URL: Article
    DOI: 10.3847/1538-3881/abbef4
    RVK:
    US 1090
    Language: Unknown
    Publisher: American Astronomical Society
    Publication Date: 2020
    detail.hit.zdb_id: 127191-X
    detail.hit.zdb_id: 2003104-X
    SSG: 16,12
    Location Call Number Limitation Availability
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    Online Resource
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