Orbital Parameters of the Eclipsing Detached Kepler Binaries with Eccentric Orbits

Kjurkchieva, D.; Vasileva, D.; Atanasova, Teodora

doi:10.3847/1538-3881/aa83b3

Cited by 32 publications

(34 citation statements)

References 57 publications

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“…The values are collected from the same RV studies from mass comparison, plotted inFig. 12, and we supplement additional eccentricity estimates from(Kjurkchieva et al 2017). While the masses of red giant components(Gaulme et al 2016) were poorly inferred, the absolute radii show good fidelity to literature values.…”

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confidence: 95%

Modelling Kepler eclipsing binaries: homogeneous inference of orbital and stellar properties

Windemuth

Agol

Ali

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We report on the properties of eclipsing binaries from the Kepler mission with a newly developed photometric modeling code, which uses the light curve, spectral energy distribution of each binary, and stellar evolution models to infer stellar masses without the need for radial velocity measurements. We present solutions and posteriors to orbital and stellar parameters for 728 systems, forming the largest homogeneous catalogue of full Kepler binary parameter estimates to date. Using comparisons to published radial velocity measurements, we demonstrate that the inferred properties (e.g., masses) are reliable for well-detached main-sequence binaries, which make up the majority of our sample. The fidelity of our inferred parameters degrades for a subset of systems not well described by input isochrones, such as short-period binaries that have undergone interactions, or binaries with post-main sequence components. Additionally, we identify 35 new systems which show evidence of eclipse timing variations, perhaps from apsidal motion due to binary tides or tertiary companions. We plan to subsequently use these models to search for and constrain the presence of circumbinary planets in Kepler eclipsing binary systems.

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confidence: 95%

Modelling Kepler eclipsing binaries: homogeneous inference of orbital and stellar properties

Windemuth

Agol

Ali

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…The places on the period-eccentricity diagram of all 32 Kepler binaries we have so far studied (Kjurkchieva & Vasileva 2015a, (Kjurkchieva & Vasileva 2015b reveal the following trends ( Figure 8): (i) There is a fast increase of the eccentricity (up to 0.57) with the period for targets with periods of 4 days < P < 25 days; (ii) there is a second increase of eccentricity beginning from e = 0.1 for periods P ≥ 35 days; and (iii) there are no targets with periods within 25-35 days, which may mean the existence of a short stage of evolution of binaries connected with a fast change of their orbits.…”

Section: Location On the Diagram Period-eccentricitymentioning

confidence: 99%

Light Curve Solutions of 12 Eccentric Kepler Binaries and Analysis of Their Out-of-Eclipse Variability

Kjurkchieva

Vasileva

Dimitrov

2016

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The eccentricity, periastron angle, orbital inclination, mass ratio, stellar temperatures and relative stellar radii of 12 eclipsing eccentric binaries were determined on the basis of Kepler data. The analysis of their out-of-eclipse variability led to the following results: (i) KIC 10490980 exhibits rotational (spottype) variability; (ii) Four new heartbeat stars were found: KIC 9344623 and KIC 10296163, which have wide tidally induced light humps and KIC 9119405 and KIC 9673173, which have narrow "Wshape" features; (iii) KIC 4932691 shows oscillations with approximately the 18th harmonic of the orbital period. We established that the eccentric Kepler binaries fall below the envelope P (1 − e 2 ) 3/2 ≈ 5 days on the period-eccentricity diagram and that there is a surprising lack of eccentric binaries with periods of 25-35 days.

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“…We therefore think that our result is more robust than the previous work. As a comparison, Kjurkchieva & Vasileva (2015) derived the orbital parameters of two binaries in the Kepler field with the W-D code and compared the parameters with those derived via EBAI by Slawson et al (2011). The two results do not match each other.…”

Section: Cstar055495mentioning

confidence: 99%

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

Liu

Zong

et al. 2018

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Based on spectroscopic observations for the eclipsing binaries CSTAR036162 and CSTAR055495 with the WiFeS/2.3 m telescope at SSO and CSTAR057775 with the Mage/MagellanI at LCO in 2017, stellar parameters are derived. More than 100 nights of almost-continuous light curves reduced from the time-series photometric observations by CSTAR at Dome A of Antarctic in i in 2008 and in g and r in 2009, respectively, are applied to find photometric solutions for the three binaries with the Wilson-Devinney code. The results show that CSTAR036162 is a detached configuration with the mass ratio q=0.354±0.0009, while CSTAR055495 is a semi-detached binary system with the unusual q=0.946±0.0006, which indicates that CSTAR055495 may be a rare binary system with mass ratio close to one and the secondary component filling its Roche Lobe. This implies that a mass-ratio reversal has just occurred and CSTAR055495 is in a rapid mass-transfer stage. Finally, CSTAR057775 is believed to be an A-type WUMa binary with q=0.301±0.0008 and a fill-out factor of f=0.742(8).

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Orbital Parameters of the Eclipsing Detached Kepler Binaries with Eccentric Orbits

Cited by 32 publications

References 57 publications

Modelling Kepler eclipsing binaries: homogeneous inference of orbital and stellar properties

Modelling Kepler eclipsing binaries: homogeneous inference of orbital and stellar properties

Light Curve Solutions of 12 Eccentric Kepler Binaries and Analysis of Their Out-of-Eclipse Variability

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

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