The Catalogue of Stellar Parameters from the Detached Double-Lined Eclipsing Binaries in the Milky Way

Eker, Z.; Bilir, S.; Soydugan, F.; Gökçe, E. Yaz; Soydugan, E.; Tüysüz, M.; Šenyüz, T.; Demirçan, Osman

doi:10.1017/pasa.2014.17

Cited by 63 publications

(49 citation statements)

References 39 publications

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“…If true, the secondary component would have a significantly inflated radius compared to predictions for mainsequence stars of that mass and age, by well over a factor of two. We note that T-Cyg1-12664 also appears in the Kepler Eclipsing Binary Catalog Slawson et al 2011) but without stellar mass or radius determinations, and also in a catalog by Eker et al (2014), but with masses and radii similar to Çakırlı et al (2013).…”

Section: Introductionsupporting

confidence: 60%

Magnetic Inflation and Stellar Mass. I. Revised Parameters for the Component Stars of the Kepler Low-mass Eclipsing Binary T-Cyg1-12664

Han

Muirhead

Swift³

et al. 2017

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Several low-mass eclipsing binary stars show larger than expected radii for their measured mass, metallicity, and age. One proposed mechanism for this radius inflation involves inhibited internal convection and starspots caused by strong magnetic fields. One particular eclipsing binary, T-Cyg1-12664, has proven confounding to this scenario. Çakırlı et al. measured a radius for the secondary component that is twice as large as model predictions for stars with the same mass and age, but a primary mass that is consistent with predictions. Iglesias-Marzoa et al. independently measured the radii and masses of the component stars and found that the radius of the secondary is not in fact inflated with respect to models, but that the primary is, which is consistent with the inhibited convection scenario. However, in their mass determinations, Iglesias-Marzoa et al. lacked independent radial velocity measurements for the secondary component due to the star's faintness at optical wavelengths. The secondary component is especially interesting, as its purported mass is near the transition from partially convective to a fully convective interior. In this article, we independently determined the masses and radii of the component stars of T-Cyg1-12664 using archival Kepler data and radial velocity measurements of both component stars obtained with IGRINS on the Discovery Channel Telescope and NIRSPEC and HIRES on the Keck Telescopes. We show that neither of the component stars is inflated with respect to models. Our results are broadly consistent with modern stellar evolutionary models for main-sequence M dwarf stars and do not require inhibited convection by magnetic fields to account for the stellar radii.

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Section: Introductionsupporting

confidence: 60%

Magnetic Inflation and Stellar Mass. I. Revised Parameters for the Component Stars of the Kepler Low-mass Eclipsing Binary T-Cyg1-12664

Han

Muirhead

Swift³

et al. 2017

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“…Moreover, if we measure the effective temperatures, we can then estimate the luminosities of the individual components (Torres et al 2010). Binary systems in close proximity are elongated toward each other because of mutual gravity; therefore, it is preferable to study only detached binaries where such effects are negligible (see Eker et al 2014). 3.…”

Section: Data Samplementioning

confidence: 99%

“…The most significant contributions come from Eker et al (2014), with 222 stars, and Serenelli et al (2017), with 397 stars. The MS/post-MS classification was done using the evolutionary tracks described in Rodrigues et al (2017), with solar metallicity.…”

Section: Data Samplementioning

confidence: 99%

Empirical Relations for the Accurate Estimation of Stellar Masses and Radii

Moya

Zuccarino

Chaplin

et al. 2018

ApJS

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In this work, we have taken advantage of the most recent accurate stellar characterizations carried out using asteroseismology, eclipsing binaries and interferometry to evaluate a comprehensive set of empirical relations for the estimation of stellar masses and radii. We have gathered a total of 934 stars-of which around two-thirds are on the main sequence-that are characterized with different levels of precision, most of them having estimates of M, R, T eff , L, g, ρ, and [Fe/H]. We have deliberately used a heterogeneous sample (in terms of characterizing techniques and spectroscopic types) to reduce the influence of possible biases coming from the observation, reduction, and analysis methods used to obtain the stellar parameters. We have studied a total of 576 linear combinations of T eff , L, g, ρ, and [Fe/H] (and their logarithms) to be used as independent variables to estimate M or R. We have used an error-in-variables linear regression algorithm to extract the relations and to ensure the fair treatment of the uncertainties. We present a total of 38 new or revised relations that have an adj-R 2 regression statistic higher than 0.85, and a relative accuracy and precision better than 10% for almost all the cases. The relations cover almost all the possible combinations of observables, ensuring that, whatever list of observables is available, there is at least one relation for estimating the stellar mass and radius.

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“…We made an extensive search for suitable systems in the literature using the SIM-BAD database (Wenger et al 2000) and NASA ADS. Useful guidance in this measure is provided by the compilations done by Kruszewski & Semeniuk (1999), Bilir et al (2008), Torres et al (2010) and more recently by Eker et al (2014), Southworth (2015) and Stassun & Torres (2016a). The final sample contains 34 systems and additionally AL Ari, a system for which our new analysis is as-yet unpublished (Konorski et al 2017).…”

Section: Introductionmentioning

confidence: 99%

The Surface Brightness-color Relations Based on Eclipsing Binary Stars: Toward Precision Better than 1% in Angular Diameter Predictions

Graczyk

Konorski

Pietrzyński

et al. 2017

ApJ

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In this study we investigate the calibration of surface brightness-color (SBC) relations based solely on eclipsing binary stars. We selected a sample of 35 detached eclipsing binaries with trigonometric parallaxes from Gaia DR1 or Hipparcos, whose absolute dimensions are known with an accuracy better than 3% and that lie within 0.3 kpc from the Sun. For the purpose of this study, we used mostly homogeneous optical and near-infrared photometry based on the Tycho-2 and 2MASS catalogs. We derived geometric angular diameters for all stars in our sample with a precision better than 10%, and for 11 of them with a precision better than 2%. The precision of individual angular diameters of the eclipsing binary components is currently limited by the precision of the geometric distances (∼5% on average). However, by using a subsample of systems with the best agreement between their geometric and photometric distances, we derived the precise SBC relations based only on eclipsing binary stars. These relations have precisions that are comparable to the best available SBC relations based on interferometric angular diameters, and they are fully consistent with them. With very precise Gaia parallaxes becoming available in the near future, angular diameters with a precision better than 1% will be abundant. At that point, the main uncertainty in the total error budget of the SBC relations will come from transformations between different photometric systems, disentangling of component magnitudes, and for hot OB stars, the main uncertainty will come from the interstellar extinction determination. We argue that all these issues can be overcome with modern high-quality data and conclude that a precision better than 1% is entirely feasible.

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The Catalogue of Stellar Parameters from the Detached Double-Lined Eclipsing Binaries in the Milky Way

Cited by 63 publications

References 39 publications

Magnetic Inflation and Stellar Mass. I. Revised Parameters for the Component Stars of the Kepler Low-mass Eclipsing Binary T-Cyg1-12664

Magnetic Inflation and Stellar Mass. I. Revised Parameters for the Component Stars of the Kepler Low-mass Eclipsing Binary T-Cyg1-12664

Empirical Relations for the Accurate Estimation of Stellar Masses and Radii

The Surface Brightness-color Relations Based on Eclipsing Binary Stars: Toward Precision Better than 1% in Angular Diameter Predictions

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