Orbital and physical parameters of eclipsing binaries from the ASAS catalogue – IX. Spotted pairs with red giants

Ratajczak, M.; Hełminiak, K. G.; Konacki, Maciej; Smith, A. M. S.; Kozłowski, S; Espinoza, N.; Jordán, Andrés; Brahm, R.; Hempel, M.; Anderson, D. R.; Hellier, C.

doi:10.1093/mnras/stw1448

Cited by 4 publications

(2 citation statements)

References 74 publications

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“…While the Galactic bulge systems do not have their spectroscopy done so far, many of the ASAS ones from Lee (2015) have their parameters published (e.g. Dimitrov et al 2014;Djurašević et al 2011;He lminiak et al 2009He lminiak et al , 2015aRatajczak et al 2013Ratajczak et al , 2016Różyczka et al 2013). …”

Section: Comparison With the Tres Resultsmentioning

confidence: 99%

HIDES spectroscopy of bright detached eclipsing binaries from the Kepler field – II. Double- and triple-lined objects

Hełminiak

Ukita

Kambe

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present the results of our spectroscopic observations of eight detached eclipsing binaries (DEBs), selected from the Kepler Eclipsing Binary Catalog. Radial velocities (RVs) were calculated from high resolution spectra obtained with the HIDES spectrograph, attached to the 1.88-m telescope of the Okayama Astrophysical Observatory, and were used to characterize the targets in combination with the Kepler light curves. For each binary we obtained a full set of orbital and physical parameters, reaching precision below 3% in masses and radii for 5 pairs. By comparing our results with theoretical models, we assess the distance, age and evolutionary status of the researched objects. We also study eclipse timing variations of selected objects, and identify a new system with a γDor pulsator. Two systems are triples, and show lines coming from three components. In one case the motion of the outer star and the perturbation in the RVs of the inner binary are clearly visible and periodical, which allows us to directly calculate the mass of the third star, and inclination of the outer orbit. In the second case we only see a clear motion of the tertiary, and investigate two scenarios: that it is a linear trend coming from the orbital motion around the inner binary, and that it is caused by a planetary mass companion. When possible, we also compare our results with the literature, and conclude that only by combining photometry with RVs it is possible to obtain correct physical parameters of both components of a DEB.

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Section: Comparison With the Tres Resultsmentioning

confidence: 99%

HIDES spectroscopy of bright detached eclipsing binaries from the Kepler field – II. Double- and triple-lined objects

Hełminiak

Ukita

Kambe

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…The fundamental parameters of detached binary stars have recently been compiled by Eker et al (2018). Their catalog consists of the data of 586 components studied in the years 1975-2017(see, e.g., Griffin & Griffin 2009Zola et al 2014;Bastürk et al 2015;Özdarcan et al 2016;Ratajczak et al 2016;Torres et al 2017). I used only the data in the catalog with mass measurements accurate to <15%.…”

Section: Comparison With Observationsmentioning

confidence: 99%

Mass–effective temperature–surface gravity relation for intermediate-mass main-sequence stars

Kílíçoǧlu

2021

A&A

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Context. In this work a mass–effective temperature–surface gravity relation (MTGR) is developed for main-sequence stars in the range 6400 K ≤ Teff ≤ 20 000 K with log g ≳ 3.44. The MTGR allows the simple estimation of the masses of stars from their effective temperatures and surface gravities. It can be used for solar metallicity and can be rescaled for any metallicity within −1.0 ≤ [Fe/H] ≤ 0.7. The effect of α-enhanced compositions can also be considered with the help of correction terms. Aims. It is aimed to develop an MTGR that can estimate the masses of main-sequence stars from their atmospheric parameters. One advantage of an MTGR over the classical mass–luminosity relations is that its mass estimation is based on parameters that can be obtained by purely spectroscopic methods, and, therefore, the interstellar extinction or reddening do not have to be known. The use of surface gravity (g) also relates an MTGR with stellar evolution and provides a more reliable mass estimation. Methods. A synthetical MTGR is obtained from theoretical isochrones using a Levenberg-Marquardt χ2 minimization algorithm. The validity of the MTGR is then checked by testing over 278 binary components with precise absolute masses. Results. Very good agreement has been obtained between the absolute masses of 278 binary star components and their masses estimated from the MTGR. A mathematical expression is also given to calculate the propagated uncertainties of the MTGR masses. Conclusions. For the typical uncertainties in atmospheric parameters and metallicity (i.e., ±2.8% for Teff, ±0.1 dex for log g and ±0.15 dex for [Fe/H]) the typical uncertainties in the masses estimated from the MTGR mostly remain around 5–9%. The fact that this uncertainty level is only on average about three times as large as that of the absolute masses indicates that the MTGR is a very powerful tool for stellar mass estimation. A computer code, mtgr.pro, written in GDL or IDL is also provided for the relation.

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Orbital and physical parameters of eclipsing binaries from the ASAS catalogue – XI. CHIRON investigation of long-period binaries

Ratajczak

Pawłaszek

Hełminiak

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present the results of a spectroscopic campaign on eclipsing binaries with long orbital period (P = 20 − 75 d) carried out with the CHIRON spectrograph. Physical and orbital solutions for seven systems were derived from the V-band, and I-band ASAS, WASP, and TESS photometry, while radial velocities were calculated from high quality optical spectra using a two-dimensional cross-correlation technique. The atmospheric parameters of the stars have been determined from the separated spectra. Most of our targets are composed of evolved stars (sub-giants or red giants) but two systems show components in different phases of evolution and one possible merger. For four binaries the masses and radii of the components were obtained with precision better than $3\%$. These objects provide very valuable information on stellar evolution.

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Orbital and physical parameters of eclipsing binaries from the ASAS catalogue – IX. Spotted pairs with red giants

Cited by 4 publications

References 74 publications

HIDES spectroscopy of bright detached eclipsing binaries from the Kepler field – II. Double- and triple-lined objects

HIDES spectroscopy of bright detached eclipsing binaries from the Kepler field – II. Double- and triple-lined objects

Mass–effective temperature–surface gravity relation for intermediate-mass main-sequence stars

Orbital and physical parameters of eclipsing binaries from the ASAS catalogue – XI. CHIRON investigation of long-period binaries

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