Photometric Solutions of Three Eclipsing Binary Stars Observed from Dome A, Antarctica

Liu, N.; Fu, J. N.; Zong, Weikai; Wang, Lizhao; Uddin, S. A.; Zhang, X. B.; Zhang, Y. P.; Cang, Tianqi; Li, G.; Yang, Yi; Grace, Yang,; Mould, Jeremy; Morrell, N.

doi:10.3847/1538-3881/aab266

Cited by 4 publications

(3 citation statements)

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“…In addition, by studying eclipse timing variations for semi-detached and contact systems, they identified two interesting triple systems and derived the orbital parameters of the third body in one system. Another detailed study on CSTAR eclipsing binaries focused on three individual objects (Liu et al 2018b).…”

Section: Variable Starsmentioning

confidence: 99%

Astronomy from Dome A in Antarctica

Shang

2020

Res. Astron. Astrophys.

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Dome A in Antarctica has been demonstrated to be the best site on earth for optical, infrared, and terahertz astronomical observations by more and more evidence, such as excellent free-atmosphere seeing, extremely low perceptible water vapor, low sky background, and continuous dark time, etc. In this paper, we present a complete picture of the development of astronomy at Dome A from the very beginning, review recent progress in time-domain astronomy, demonstrate exciting results of the site testing, and address the challenges in instrumentation. Currently proposed projects are briefly discussed.

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Section: Variable Starsmentioning

confidence: 99%

Astronomy from Dome A in Antarctica

Shang

2020

Res. Astron. Astrophys.

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“…Even if some binaries with large mass ratio (i.e., unequal masses) have a period shorter than the upper-period limit, they will fail to produce a long-lived W UMa binaries due to case AD evolution, e.g. WY Cnc (P ∼ 0.83, q ∼ 2.61, Heckert et al 1998;Chen 2013), CSTAR 036162 (P ∼ 0.87d, q ∼ 2.82, Liu et al 2018). However, they may be the best candidates of the commonenvelope merger, and can also be used to constrain adiabatic mass-loss models in binaries (Ge et al 2010).…”

Section: The Progenitors Of W Uma Binariesmentioning

confidence: 99%

Case AD, AR, and AS binary evolution and their possible connections with W UMa binaries

Jiang

2019

Monthly Notices of the Royal Astronomical Society

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Close detached binaries were theoretically predicted to evolve into contact by three subtypes of case A binary evolution: case AD, AR, and AS, which correspond to the formation of contact during dynamic-, thermal-, and nuclear-timescale mass transfer phase, respectively. It is unclear, however, what is the difference between contact binaries in these subtypes, and whether all of these subtypes can account for the formation of observed W UMa binaries. Using Eggleton's stellar evolution code with the nonconservative assumption, I obtained the low-mass contact binaries produced by case AD, AR, and AS at the moment of contact, and their parameter spaces. The results support that the progenitors of low-mass contact binaries are detached binaries with orbital periods shorter than ∼ 2 − 5 d, and their borderlines depend strongly on the primary mass. In addition, the period-colour relations for case AR and AS can be in better agreement with that for observed W UMa candidates, but case AD shows a significantly worse agreement. Moreover, case AR and AS can produce a short-period limit (corresponding to a low-mass limit) at almost any age, e.g. from young age (∼ 0.2 Gyr) to old age (∼ 13 Gyr), agreeing with observed W UMa binaries in star clusters, but no such limit occurs for case AD at any age. These results support that case AR and AS, as opposed to case AD, can lead to W UMa binaries (including young W UMa binaries).

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“…There are a number of tailored approaches that have been implemented for binary identification in the field, such as interferometry (e.g Raghavan et al 2010),. eclipsing transits (e.g Qian et al 2017;Zhang et al 2017;Liu et al 2018;Yang et al 2020),. color displacements (e.g Pourbaix et al 2004;Yuan et al 2015a),.…”

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confidence: 99%

Data-driven spectroscopic estimates of absolute magnitude, distance and binarity -- method and catalog of 16,002 O- and B-type stars from LAMOST

Xiang,

Rix,

Ting

et al. 2020

Preprint

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We present a data-driven method to estimate absolute magnitudes for O-and B-type stars from the LAMOST spectra, which we combine with Gaia parallaxes to infer distance and binarity. The method applies a neural network model trained on stars with precise Gaia parallax to the spectra and predicts K s -band absolute magnitudes M Ks with a precision of 0.25 mag, which corresponds to a precision of 12% in spectroscopic distance. For distant stars (e.g. > 5 kpc), the inclusion of constraints from spectroscopic M Ks significantly improves the distance estimates compared to inferences from Gaia parallax alone. Our method accommodates for emission line stars by first identifying them via PCA reconstructions and then treating them separately for the M Ks estimation. We also take into account unresolved binary/multiple stars, which we identify through deviations in the spectroscopic M Ks from the geometric M Ks inferred from Gaia parallax. This method of binary identification is particularly efficient for unresolved binaries with near equalmass components and thus provides an useful supplementary way to identify unresolved binary or multiple-star systems. We present a catalog of spectroscopic M Ks , extinction, distance, flags for emission lines, and binary classification for 16,002 OB stars from LAMOST DR5. As an illustration of the method, we determine the M Ks and distance to the enigmatic LB-1 system, where Liu et al. (2019a) had argued for the presence of a black hole and incorrect parallax measurement, and we do not find evidence for errorneous Gaia parallax.

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Photometric Solutions of Three Eclipsing Binary Stars Observed from Dome A, Antarctica

Cited by 4 publications

References 50 publications

Astronomy from Dome A in Antarctica

Astronomy from Dome A in Antarctica

Case AD, AR, and AS binary evolution and their possible connections with W UMa binaries

Data-driven spectroscopic estimates of absolute magnitude, distance and binarity -- method and catalog of 16,002 O- and B-type stars from LAMOST

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