The eccentric massive binary V380 Cyg: revised orbital elements and interpretation of the intrinsic variability of the primary component*

Tkachenko, A.; Degroote, P.; Aerts, C.; Pavlovski, K.; Southworth, J.; Pápics, P. I.; Moravveji, E.; Kolbas, V.; Tsymbal, V.; Debosscher, J.; Clémer, K.

doi:10.1093/mnras/stt2421

Cited by 70 publications

(100 citation statements)

References 70 publications

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“…This is in agreement with results on a sample of massive DEBs (Pavlovski & Hensberge 2005;Pavlovski & Southworth 2009Pavlovski et al , 2011Mayer et al 2013;Tkachenko et al 2014, with typical v rot sin i 100 km s −1 ), which also show no signs of mixing with CN-cycled matter. Mixing signatures are found in the remaining 1/3 of our sample stars.…”

Section: Evolutionary Status Of the Sample Starssupporting

confidence: 91%

“…The most accurate and precise fundamental parameters for massive stars available at present can be found in the compilation by Torres et al (2010, henceforth abbreviated TAG10), mainly for the most common among them, the early B-type stars of spectral types B0 to B3. Data on abundances of individual chemical elements in massive DEBs are scarce, though ongoing projects promise to alleviate the situation (Pavlovski & Hensberge 2005;Pavlovski & Southworth 2009Pavlovski et al , 2011Mayer et al 2013;Tkachenko et al 2014). …”

Section: Introductionmentioning

confidence: 99%

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Fundamental properties of nearby single early B-type stars

Nieva

Przybilla

2014

A&A

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Aims. Fundamental parameters of a sample of 26 apparently slowly-rotating single early B-type stars in OB associations and in the field within a distance of 400 pc from the Sun are presented and compared to high-precision data from detached eclipsing binaries (DEBs). Together with surface abundances for light elements the data are used to discuss the evolutionary status of the stars in context of the most recent Geneva grid of models for core hydrogen-burning stars in the mass-range ∼6 to 18 M at metallicity Z = 0.014. Methods. The fundamental parameters are derived on the basis of accurate and precise atmospheric parameters determined earlier by us from non-LTE analyses of high-quality spectra of the sample stars, utilising the new Geneva stellar evolution models. Results. Evolutionary masses plus radii and luminosities are determined to better than typically 5%, 10%, and 20% uncertainty, respectively, facilitating the mass−radius and mass−luminosity relationships to be recovered for single core hydrogen-burning objects with a similar precision as derived from DEBs. Good agreement between evolutionary and spectroscopic masses is found. Absolute visual and bolometric magnitudes are derived to typically ∼0.15−0.20 mag uncertainty. Metallicities are constrained to better than 15−20% uncertainty and tight constraints on evolutionary ages of the stars are provided. Overall, the spectroscopic distances and ages of individual sample stars agree with independently derived values for the host OB associations. Signatures of mixing with CN-cycled material are found in 1/3 of the sample stars. Typically, these are consistent with the amount predicted by the new Geneva models with rotation. The presence of magnetic fields appears to augment the mixing efficiency. In addition, a few objects are possibly the product of binary evolution. In particular, the unusual characteristics of τ Sco point to a blue straggler nature, due to a binary merger. Conclusions. The accuracy and precision achieved in the determination of fundamental stellar parameters from the quantitative spectroscopy of single early B-type stars comes close (within a factor 2-4) to data derived from DEBs. While our fundamental parameters are in good agreement with those derived from DEBs as a function of spectral type, significant systematic differences with data from the astrophysical reference literature are found. Masses are ∼10−20% and radii ∼25% lower then the recommended values for luminosity class V, resulting in the stars being systematically fainter than assumed usually, by ∼0.5 mag in absolute visual and bolometric magnitude. Our sample of giants is too small to derive firm conclusions, but similar trends as for the dwarfs are indicated.

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Section: Evolutionary Status Of the Sample Starssupporting

confidence: 91%

Section: Introductionmentioning

confidence: 99%

Fundamental properties of nearby single early B-type stars

Nieva

Przybilla

2014

A&A

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“…A study of the correlation between α ov and mass by Ribas et al (2000) used a total of eight DLEBs with component masses in the range 2-12 M , and found a strong dependence of the extra mixing on mass. These authors relied very heavily on the massive binary V380 Cyg (M 1 ∼ 11 M , M 2 ∼ 7 M ) to establish the slope of the relation, however, fitting the measured properties of this critical system has always been problematic, as discussed at length by Claret (2007) and also more recently by Tkachenko et al (2014). The latter authors reported a new set of precise determinations of the mass, radius, temperature, chemical composition, and other properties of the components that have nevertheless remained difficult to reconcile with models.…”

Section: Introductionmentioning

confidence: 99%

The dependence of convective core overshooting on stellar mass

Claret

Torres

2016

A&A

104

118

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Context. Convective core overshooting extends the main-sequence lifetime of a star. Evolutionary tracks computed with overshooting are very different from those that use the classical Schwarzschild criterion, which leads to rather different predictions for the stellar properties. Attempts over the last two decades to calibrate the degree of overshooting with stellar mass using detached double-lined eclipsing binaries have been largely inconclusive, mainly because of a lack of suitable observational data. Aims. We revisit the question of a possible mass dependence of overshooting with a more complete sample of binaries, and examine any additional relation there might be with evolutionary state or metal abundance Z. Methods. We used a carefully selected sample of 33 double-lined eclipsing binaries strategically positioned in the H-R diagram with accurate absolute dimensions and component masses ranging from 1.2 to 4.4 M . We compared their measured properties with stellar evolution calculations to infer semi-empirical values of the overshooting parameter α ov for each star. Our models use the common prescription for the overshoot distance d ov = α ov H p , where H p is the pressure scale height at the edge of the convective core as given by the Schwarzschild criterion, and α ov is a free parameter. Results. We find a relation between α ov and mass, which is defined much more clearly than in previous work, and indicates a significant rise up to about 2 M followed by little or no change beyond this mass. No appreciable dependence is seen with evolutionary state at a given mass, or with metallicity at a given mass although the stars in our sample span a range of a factor of ten in [Fe/H], from −1.01 to +0.01.

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“…In particular, the authors found that the position of the more evolved primary component in the Kiel diagram can only be explained when a large amount of extra mixing in terms of the overextension of the convective core (core overshoot α) is included in the models. The system has been recently revisited by [31] based on high-quality space-based Kepler photometry and ground-based, highresolution hermes [27] spectroscopy. The authors found that the evolutionary tracks computed for the dynamical masses of the stars fail to explain their positions in the Kiel diagram (see Fig.…”

Section: Mass Discrepancymentioning

confidence: 99%

“…Thanks to the fact that many pulsating stars are found in binary systems across the whole HR-diagram, binary stars -systems consisting of two stellar objects that periodically revolve around their common center of mass -can provide us with additional, model-independent observational constraints in terms of the dynamical masses and radii of stars. Nowadays, we talk about dynamical measurements of fundamental properties of stars in large mass and age ranges to precisions approaching 1% [e.g., 15,31]. This way, asteroseismic investigations can be confronted/supplied with model-independent fundamental properties of stars, providing a valuable test of the current theories of stellar structure and evolution.…”

Section: Introductionmentioning

confidence: 99%

Dynamical Asteroseismology: towards improving the theories of stellar structure and (tidal) evolution

Tkachenko

2017

EPJ Web Conf.

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Abstract. The potential of the dynamical asteroseismology, the research area that builds upon the synergies between the asteroseismology and binary stars research fields, is discussed in this manuscript. We touch upon the following topics: i) the mass discrepancy observed in intermediate-to high-mass main-sequence and evolved binaries as well as in the low mass systems that are still in the pre-main sequence phase of their evolution; ii) the rotationally induced mixing in high-mass stars, in particular how the most recent theoretical predictions and spectroscopic findings compare to the results of asteroseismic investigations; iii) internal gravity waves and their potential role in the evolution of binary star systems and surface nitrogen enrichment in high-mass stars; iv) the tidal evolution theory, in particular how its predictions of spin-orbit synchronisation and orbital circularisation compare to the present-day high-quality observations; v) the tidally-induced pulsations and their role in the angular momentum transport within binary star systems; vi) the scaling relations between fundamental and seismic properties of stars across the entire HR-diagram.

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The eccentric massive binary V380 Cyg: revised orbital elements and interpretation of the intrinsic variability of the primary component*

Cited by 70 publications

References 70 publications

Fundamental properties of nearby single early B-type stars

Fundamental properties of nearby single early B-type stars

The dependence of convective core overshooting on stellar mass

Dynamical Asteroseismology: towards improving the theories of stellar structure and (tidal) evolution

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