Orbital and physical parameters of eclipsing binaries from the All-Sky Automated Survey catalogue

Hełminiak, K. G.; Tokovinin, Andreï; Niemczura, E.; Pawłaszek, Rafał; Yanagisawa, K.; Brahm, R.; Espinoza, N.; Ukita, Nobuharu; Kambe, Eiji; Ratajczak, M.; Hempel, M.; Jordán, Andrés; Konacki, Maciej; Sybilski, P.; Kozłowski, S; Litwicki, M.; Tamura, Motohide

doi:10.1051/0004-6361/201732482

Cited by 14 publications

(7 citation statements)

References 111 publications

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“…The disentangling typically provides spectra of the fainter components with a higher S/N, which can be used for spectroscopic analysis. The advantages and limitations of the above techniques are discussed in detail by, e.g., Ilijic (2004) or Hełminiak et al (2019).…”

Section: Disentangling Spectra With Korelmentioning

confidence: 99%

HD 183986: A High-contrast SB2 System with a Pulsating Component

Vaňko

Pribulla

Gajdoš

et al. 2022

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There is a small group of peculiar early-type stars on the main sequence that show different rotation velocities from different spectral lines. This inconsistency might be due to the binary nature of these objects. We aim to verify this hypothesis by a more detailed spectroscopic and photometric investigation of one such object: HD 183986. We obtained 151 high- and medium-resolution spectra that covered an anticipated long orbital period. There is clear evidence of the orbital motion of the primary component. We uncovered a very faint and broad spectrum of the secondary component. The corresponding SB2 orbital parameters, and the component spectra, were obtained by Fourier disentangling using the KOREL code. The component spectra were further modeled by iSpec code to arrive at the atmospheric quantities and the projected rotational velocities. We have proven that this object is a binary star with a period P = 1268.2(11) days, eccentricity e = 0.5728(20), and mass ratio q = 0.655. The primary component is a slowly rotating star ( v sin i = 27 km s−1) while the cooler and less massive secondary rotates much faster ( v sin i ∼ 120 km s−1). Photometric observations obtained by the Transiting Exoplanet Survey Satellite (TESS) satellite were also investigated to shed more light on this object. A multiperiod photometric variability was detected in the TESS data ranging from hours (the δ Sct-type variability) to a few days (spots/rotational variability). The physical parameters of the components and the origin of the photometric variability are discussed in more detail.

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Section: Disentangling Spectra With Korelmentioning

confidence: 99%

HD 183986: A High-contrast SB2 System with a Pulsating Component

Vaňko

Pribulla

Gajdoš

et al. 2022

View full text Add to dashboard Cite

show abstract

“…The disentangling typically provides spectra of the fainter components with a higher SNR, which can be used for spectroscopic analysis. The advantages and limitations of the above techniques are discussed in detail by e.g., Ilijic (2004) or Hełminiak et al (2019).…”

Section: Disentangling Spectra With Korelmentioning

confidence: 99%

HD 183986: a high-contrast SB2 system with a pulsating component

Vaňko,

Pribulla,

Gajdoš

et al. 2022

Preprint

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There is a small group of peculiar early-type stars on the main sequence that show different rotation velocities from different spectral lines. This inconsistency might be due to the binary nature of these objects. We aim to verify this hypothesis by a more detailed spectroscopic and photometric investigation of one such object: HD 183986. We obtained 151 high and medium resolution spectra that covered an anticipated long orbital period. There is clear evidence of the orbital motion of the primary component. We uncovered a very faint and broad spectrum of the secondary component. The corresponding SB2 orbital parameters, and the component spectra, were obtained by Fourier disentangling using the KOREL code. The component spectra were further modeled by iSpec code to arrive at the atmospheric quantities and the projected rotational velocities. We have proven that this object is a binary star with the period P = 1268.2(11) d, eccentricity e = 0.5728(20), and mass ratio q = 0.655. The primary component is a slowly rotating star (v sin i = 27 km s −1 ) while the cooler and less massive secondary rotates much faster (v sin i ∼ 120 km s −1 ). Photometric observations obtained by the TESS satellite were also investigated to shed more light on this object. A multi-period photometric variability was detected in the TESS data ranging from hours (the δ Sct-type variability) to a few days (spots/rotational variability). The physical parameters of the components and the origin of the photometric variability are discussed in more detail.

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“…-ASAS J065134-2211,5: Hełminiak et al (2019b) presents the orbital and physical parameters of this binary. Concerning the analysis by means of stellar models, they use the PARSEC code from Marigo et al (2017) and they fit the primary star in 1σ for an isochrone of 6.3 Gyr in the observational plan {(M vs T eff ), (M vs L), (M vs R)}.…”

Section: Eclipsing Binaries Data and Model: Binary Age Determinationmentioning

confidence: 99%

“…They claim that this problem could be related to the chromospheric activity of the system. -ASAS J073507-0905,7: Hełminiak et al (2019b) also studied this binary. The analysis was preformed in the same observational plans.…”

Section: Eclipsing Binaries Data and Model: Binary Age Determinationmentioning

confidence: 99%

Revisiting the mass- and radius-luminosity relations for FGK main-sequence stars

Fernandes,

Gafeira,

Andersen

2021

Preprint

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Context. Scaling relations are very useful tools for estimating unknown stellar quantities. Within this framework, eclipsing binaries are ideal for this goal because their mass and radius are known with a very good level of accuracy, leading to improved constraints on the models. Aims. We aim to provide empirical relations for the mass and radius as function of luminosity, metallicity, and age. We investigate, in particular, the impact of metallicity and age on those relations. Methods. We used a multi-dimensional fit approach based on the data from DEBCat, an updated catalogue of eclipsing binary observations such as mass, radius, luminosity, effective temperature, gravity, and metallicity. We used the PARAM web interface for the Bayesian estimation of stellar parameters, along with the stellar evolutionary code MESA to estimate the binary age, assuming a coeval hypothesis for both members. Results. We derived the mass and radius-luminosity-metallicity-age relations using 56 stars, with metallicity and mass in the range −0.34 <[Fe/H]< 0.27 and 0.66 < M/M < 1.8. With that, the observed mass and radius are reproduced with an accuracy of 3.5% and 5.9%, respectively, which is consistent with the other results in literature. Conclusions. We conclude that including the age in such relations increases the quality of the fit, particularly in terms of the mass, as compared to the radius. On the other hand, as other authors have noted, we observed an higher dispersion on the mass relation than in that of the radius. We propose that this is due to a stellar age effect.

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Orbital and physical parameters of eclipsing binaries from the All-Sky Automated Survey catalogue

Cited by 14 publications

References 111 publications

HD 183986: A High-contrast SB2 System with a Pulsating Component

HD 183986: A High-contrast SB2 System with a Pulsating Component

HD 183986: a high-contrast SB2 system with a pulsating component

Revisiting the mass- and radius-luminosity relations for FGK main-sequence stars

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