Physical parameters of some close binaries: ET Boo, V1123 Tau, V1191 Cyg, V1073 Cyg and V357 Peg

Ekmekci, F.; Elmaslı, A.; Yılmaz, M.; Kílíçoǧlu, T.; Tanrıverdi, T.; Baştürk, Özgür; Şenavcı, H. V.; Çalışkan, Şeyma; Albayrak, B.; Selam, S. O.

doi:10.1016/j.newast.2012.03.001

Cited by 19 publications

(4 citation statements)

References 36 publications

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“…Their results are in good agreement with those presented by Deb & Singh (2011). Ekmekçi et al (2012) obtained new BVR photometric observations and derived a somewhat larger orbital inclination of i = 74 • , which resulted in slightly smaller masses than those given by Deb & Singh (2011) and Zhang et al (2011).…”

Section: V1123 Taumentioning

confidence: 78%

“…They found it to have an orbital inclination of i = 73.2 • , a contact configuration with fill-out factor of f = 10 per cent and a temperature difference between the components ∆T = 562 K. The resulting physical parameters were: M1 = 1.720 ± 0.015M ⊙ and M2 = 0.690 ± 0.013M ⊙ . Ekmekçi et al (2012) used their BV R band photometric data and the spectroscopic mass ratio from Rucinski et al (2008) and arrived at a model with a similar inclination but a higher fill-out factor (31.2 per cent). The temperatures of the components differ by 300 K. A somewhat different absolute parameters than those in Deb & Singh (2011) were determined: M1 = 0.85 ± 0.03M ⊙ and M2 = 0.34 ± 0.02M ⊙ .…”

Section: V357 Pegmentioning

confidence: 99%

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Physical parameters of close binary systems: VIII

Gazeas

Zoła

Liakos

et al. 2021

Monthly Notices of the Royal Astronomical Society

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This paper presents the results of a combined spectroscopic and photometric study of 20 contact binary systems: HV Aqr, OO Aql, FI Boo, TX Cnc, OT Cnc, EE Cet, RW Com, KR Com, V401 Cyg, V345 Gem, AK Her, V502 Oph, V566 Oph, V2612 Oph, V1363 Ori, V351 Peg, V357 Peg, Y Sex, V1123 Tau, and W UMa, which was conducted in the frame of the W UMa Project. Together with 51 already covered by the project and an additional 67 in the existing literature, these systems bring the total number of contact binaries with known combined spectroscopic and photometric solutions to 138. It was found that mass, radius, and luminosity of the components follow certain relations along the MS and new empirical power relations are extracted. We found that 30 per cent of the systems in the current sample show extreme values in their parameters, expressed in their mass ratio or fill-out factor. This study shows that, among the contact binary systems studied, some have an extremely low mass ratio (q < 0.1) or an ultrashort orbital period (Porb < 0.25 d), which are expected to show evidence of mass transfer progress. The evolutionary status of these components is discussed with the aid of correlation diagrams and their physical and orbital parameters compared to those in the entire sample of known contact binaries. The existence of very short orbital periods confirms the very slow nature of the merging process, which seems to explain why their components still exist as MS stars in contact configurations even after several Gyr of evolution.

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Section: V1123 Taumentioning

confidence: 78%

Section: V357 Pegmentioning

confidence: 99%

Physical parameters of close binary systems: VIII

Gazeas

Zoła

Liakos

et al. 2021

Monthly Notices of the Royal Astronomical Society

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show abstract

“…We also note that in the cases of three objects (SW Lac, V357 Peg, V781 Tau), physical parameters (especially the effective temperatures) adopted from the most recent analyses (Şenavcı et al 2011;Ekmekçi et al 2012;Li et al 2016, respectively) did not result in well-fitted models of our observed spectra. In these cases, we decided to adopt physical parameters from earlier studies (Gazeas et al 2005;Deb & Singh 2011;Kallrath et al 2006, respectively), which allowed us to construct better models.…”

Section: List Of Targetsmentioning

confidence: 62%

Chromospheric activity in bright contact binary stars

Mitnyan

Szalai

Bódi

et al. 2020

A&A

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Context. Studying chromospheric activity of contact binaries is an important way of revealing the magnetic activity processes of these systems. An efficient but somewhat neglected method for that is to follow the changes of the Hα line profiles via optical spectroscopy. Aims. Our goal was to perform a comprehensive preliminary analysis based on the optical spectral signs of chromospheric activity on the largest sample of contact binaries to date. Methods. We collected optical echelle spectra on 12 bright contact binaries at 17 nights. We derived new radial velocity curves from our observations. For quantifying the apparent chromospheric activity levels of the systems, we subtracted self-constructed synthetic spectra from the observed ones and measured the equivalent widths of the residual Hα-profiles at each observed epoch. Our wellsampled data set allowed us to study the short-term variations of chromospheric activity levels as well as to search for correlations between them and some basic physical parameters of the systems. Results. Fitting the radial velocity curves, we re-determined the mass ratios and systemic velocities of all observed objects. We found that chromospheric activity levels of the studied systems show various changes during the orbital revolution: we see either flat, or onepeaked, or two-peaked distributions of equivalent width vs. the orbital phase. The first case means that the activity level is probably constant, while the latter two cases suggest the presence of one or two active longitudes at the stellar surfaces. Our correlation diagrams show that mean chromospheric activity levels may be in connection with orbital periods, B−V color indices, inverse Rossby numbers, and temperature differences of the components. At the same time, no clear trend is visible with respect to mass ratios, inclinations and fill-out factors of the systems. A-and W-type contact binaries in our sample show similar distributions at each of the studied correlation diagrams.

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“…Strohmeier (1960) first recognized the variability of V1073 Cyg, then the photographic (pg) light curve was published in 1962 (Strohmeier 1962). Thus far, more photometric and spectrographic researches have been carried out for V1073 Cyg (such as Sezer 1993;Morris & Naftilan 2000;Yang & Liu 2000;Ekmekc ¸i et al 2012), and absolute parameters have been derived. Here is a brief introduction.…”

Section: Introductionmentioning

confidence: 99%

Multi-color light curves and orbital period research of eclipsing binary V1073 Cyg

Tian

Zhu

Qian

et al. 2018

Res. Astron. Astrophys.

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New Multi-color B V R c I c photometric observation are presented for W UMa type eclipsing binary V1073 Cyg. The multi-color light curves analysis with the Wilson-Devinney(W-D) procedure acquired the absolute parameters of this system, showing thatV1073Cyg is a shallow contact binary system with fill-out factor f = 0.124(±0.011). We collected all available times of light minima spanning 119 years including CCD data to construct the O-C curve and made detailed O-C analysis. The O-C diagram shows that the period change is complex. There exist a long-term continuous decrease and a cyclic variation. The period is decreasing at a rate ofṖ = −1.04(±0.18) × 10 −10 days · cycle −1 , and with the period decrease, V1073 Cyg will evolve to deep contact stage. The cyclic variation with a period of P 3 = 82.7(±3.6)years and an amplitude of A = 0.028(±0.002)day may be explained by the magnetic activity of one or both components or the light travel time effect (LTTE) caused by a distant third companion with M 3 (i ′ = 90 • ) = 0.511M ⊙ .

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Physical parameters of some close binaries: ET Boo, V1123 Tau, V1191 Cyg, V1073 Cyg and V357 Peg

Cited by 19 publications

References 36 publications

Physical parameters of close binary systems: VIII

Physical parameters of close binary systems: VIII

Chromospheric activity in bright contact binary stars

Multi-color light curves and orbital period research of eclipsing binary V1073 Cyg

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