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

Windemuth, Diana; Agol, Eric; Ali, Aleezah; Kiefer, F.

doi:10.1093/mnras/stz2137

Cited by 29 publications

(57 citation statements)

References 114 publications

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“…A related empirical method has also been used by Maxted & Hutcheon (2018) for characterizing EBs from the K2 survey. Most recently, Windemuth et al (2019) have determined physical and orbital parameters in such a manner for the detached EBs in the original Kepler field. Our method was mainly inspired by the paper of Windemuth et al (2019), however, as far as we are aware, our efforts are the first to apply the SED+isochrone fitting method for multiple stellar systems.…”

Section: J O I N T P H Y S I C a L A N D Dy Na M I C A L M O D E L L mentioning

confidence: 99%

“…During the MCMC runs, these variables were adjusted together with the mass ratio (q 1 ), the orbital elementrelated parameters (see above), the third light ( ), the extinction parameter [E(B −V)], and the distance of the actual system (d). Regarding this last item, our treatment slightly departs from that of Windemuth et al (2019). Those authors used Gaussian priors for the distance calculated from Gaia's DR2 trigonometric parallax (and its uncertainty).…”

Section: J O I N T P H Y S I C a L A N D Dy Na M I C A L M O D E L L mentioning

confidence: 99%

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TICs 167692429 and 220397947: the first compact hierarchical triple stars discovered with TESS

Borkovits

Rappaport

Hajdu

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We report the discovery and complex analyses of the first two compact hierarchical triple star systems discovered with TESS in or near its southern continuous viewing zone during Year 1. Both TICs 167692429 and 220397947 were previously unknown eclipsing binaries, and the presence of a third companion star was inferred from eclipse timing variations exhibiting signatures of strong third-body perturbations and, in the first system, also from eclipse depth variations. We carried out comprehensive analyses, including the simultaneous photodynamical modelling of TESS and archival ground-based WASP light curves, as well as eclipse timing variation curves. Also, for the first time, we included in the simultaneous fits multiple star spectral energy distribution data and theoretical PARSEC stellar isochrones, taking into account Gaia DR2 parallaxes and catalogued metallicities. We find that both systems have twin F-star binaries and a lower mass tertiary star. In the TIC 167692429 system, the inner binary is moderately inclined (imut = 27°) with respect to the outer orbit, and the binary versus outer (triple) orbital periods are 10.3 versus 331 d, respectively. The mutually inclined orbits cause a driven precession of the binary orbital plane that leads to the disappearance of binary eclipses for long intervals. In the case of TIC 220397947, the two orbital planes are more nearly aligned and the inner versus outer orbital periods are 3.5 and 77 d, respectively. In the absence of radial velocity observations, we were unable to calculate highly accurate masses and ages for the two systems. According to stellar isochrones TIC 167692429 might be either a pre-main sequence (MS) or an older post-MS system. In the case of TIC 220397947, our solution prefers a young pre-MS scenario.

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Section: J O I N T P H Y S I C a L A N D Dy Na M I C A L M O D E L L mentioning

confidence: 99%

Section: J O I N T P H Y S I C a L A N D Dy Na M I C A L M O D E L L mentioning

confidence: 99%

TICs 167692429 and 220397947: the first compact hierarchical triple stars discovered with TESS

Borkovits

Rappaport

Hajdu

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…They also provided estimates for the stellar ages, but caution that these are likely unreliable. We believe this is indeed the case -although one expects no more than ∼1% of stars in the Kepler sample to have ages younger than ∼ 10 8 years, ∼20% of the binaries in the Windemuth et al (2019) catalogue do so. In this work, we discard their age information.…”

Section: Eclipsing Binary Datamentioning

confidence: 85%

“…We are aided by results from a number of recent surveys, such as eclipsing binaries from the Kepler and TESS photometric missions (e.g. Milliman et al 2014;Van Eylen et al 2016;Triaud et al 2017;Windemuth et al 2019;Justesen & Albrecht 2021) , 2020Kounkel et al 2021). By analysing the eclipsing binary data, we find most binaries circularize interior to ∼6 days, with a sub-population of binaries circularizing interior to only ∼3 days, a conclusion which differs drastically from Meibom & Mathieu (2005).…”

Section: Introductionmentioning

confidence: 88%

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A Tale of Two Circularization Periods

Zanazzi

2021

Preprint

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We re-analyze the pristine eclipsing binary data from the Kepler and TESS missions, focusing on eccentricity measurements at short orbital periods to emperically constrain tidal circularization. We find an average circularization period of ∼6 days, as well as a short circularization period of ∼3 days for the Kepler /TESS field binaries. We argue previous spectroscopic binary surveys reported longer circularization periods due to small sample sizes, which were contaminated by an abundance of binaries with circular orbits out to ∼10 days, but we re-affirm their data shows a difference between the eccentricity distributions of young (<1 Gyr) and old (>3 Gyr) binaries. Our work calls into question the long circularization periods quoted often in the literature.

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Optimized cutting off transit algorithm to study stellar rotation from PLATO mission light curves

et al. 2020

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Measuring the stellar rotation of one of the components in eclipsing binaries (EBs) or planetary systems is a challenge task. The difficulty is mainly due to the complexity of analyzing, in the same light curve, the signal from the stellar rotation mixed with the transit signal of a stellar or substellar companion, like a brown dwarf or planet. There are many methods to correct the long-term trend of the light curve. However, the correction often erases the signal of the stellar rotation from spots crossing the visible stellar disk and other weaker signals like planets. In this work, we present the DiffeRencial flUx Method of cuTting Off biNariES (DRUM TONES) to identify the signal of the binary transits and disentangle it from stellar rotation planet signals. We present our technique with applications to EBs from CoRoT, Kepler, Kepler K2 and TESS missions. We also applied our method to simulated synthetic EB from the PLATO mission. Our method shows good agreement in the determination of stellar rotation periods for few observed targets from last space missions, as well it is naturally useful for future European mission, such as PLAnetary Transits and Oscillations of stars (PLATO).

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

Cited by 29 publications

References 114 publications

TICs 167692429 and 220397947: the first compact hierarchical triple stars discovered with TESS

TICs 167692429 and 220397947: the first compact hierarchical triple stars discovered with TESS

A Tale of Two Circularization Periods

Optimized cutting off transit algorithm to study stellar rotation from PLATO mission light curves

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