A photometric study of a weak-contact binary: V873 Per

Kriwattanawong, Wichean; Poojon, P.

doi:10.1016/j.newast.2014.10.004

Cited by 9 publications

(17 citation statements)

References 25 publications

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“…Both variations of fill-out factor and period have been found in many systems e.g., CC Com (Yang et al 2009a) and V599 Aur (Hu et al 2020). More examples e.g., V873 Per shows clearly about increasing fill-out factor from 5.5 % (Samec et al 2009) to 18.1 % (Kriwattanawong & Poojon 2015), V502 Oph e.g., f = 22 % (Deb & Singh 2011) to f = 35.3 % (Zhou et al 2016). After the evolution of BM UMa reaches the stage where mass ratio q close to 1 and goes further the point q < 1.0, the binary will evolve into A-subtype as a deeper normal overcontact binary where the mass transfer takes place from the less massive component (m 2 ) to the more massive one (m 1 ), similar to the present evolutionary stage of V802 Aql (P = 0.2677 d; Yang et al 2008) where its orbital period is increasing and the fill-out factor also gradually grows (f = 35 %) at the beginning stage of A-subtype before becoming a deep low-mass ratio overcontact system.…”

Section: Discussionmentioning

confidence: 93%

BM UMa: a middle shallow contact binary at pre-transition stage of evolution from W-type to A-type

Sarotsakulchai,

Soonthornthum,

Poshyachinda

et al. 2021

Preprint

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In this study, all unpublished time series photometric data of BM UMa (q ∼ 2.0, P = 0.2712 d) from available archives were re-investigated together with new data taken from the TNT-2.4m of the Thai National Observatory (TNO). Based on period analysis, there is a shortterm variation superimposed on the long-term period decrease. The trend of period change can be fitted with a downward parabolic curve indicating a period decrease at a rate of dP/dt = −3.36(±0.02) × 10 −8 d yr −1 . This long-term period decrease can be explained by mass transfer from the more massive component (M 2 ∼ 0.79M ) to the less massive one (M 1 ∼ 0.39M ), combination with AML. For photometric study, we found that the binary consists of K0 V stars and at the middle shallow contact phase with evolution of fill-out factor from 8.8 % (in 2007) to 23.2 % (in 2020). Those results suggest that the binary is at pre-transition stage of evolution from W-type to A-type, agreeing to the results of statistical study of W-type contact binaries. The mass of M 2 will be decreased close to or below M 1 and the mass ratio will be decreased (q < 1.0). By this way, the binary will evolve into A-type as a deeper normal

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Section: Discussionmentioning

confidence: 93%

BM UMa: a middle shallow contact binary at pre-transition stage of evolution from W-type to A-type

Sarotsakulchai,

Soonthornthum,

Poshyachinda

et al. 2021

Preprint

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“…This fact does not allow to prefer one of these periods of time of minima variations and it is possible that both of them are valid, also there is a possibility that only one of these periodical variations is real. Kriwattanawong & Poojon (2015) could not make a final conclusion about nature of the time variation and 6 Because of their mean square-error is greater than 2.5σ. We can not offer an explanation of this high deviation and suppose that it arises from data processing and algorithms of minima time finding (for example, if individual observations of light curve during those nights were performed with significantly longer breaks between points in comparison with other observations) rather than from physical processes.…”

Section: Light Equationmentioning

confidence: 99%

“…Times of light minima obtained from our own observations are shown in Table 2. These minima moments were determined in free search by solving the light curves at fixed geometrical parameters taken from previous study (Kriwattanawong & Poojon 2015) using a program 4 designed to calculate orbital elements.…”

Section: Light Equationmentioning

confidence: 99%

“…The derived contact degree was found to be f = 18.10%(±1.36%). Kriwattanawong & Poojon (2015) suspected the cyclic variation with the period of about 4 years that could be due to existence of the third companion in the system or the mechanism of magnetic activity cycle in the binary.…”

Section: Introductionmentioning

confidence: 99%

“…http://c-munipack.sourceforge.net3 We do not use moment of minimum 2451370.8753(Nicholson & Varley 2006) followingKriwattanawong & Poojon (2015).…”

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confidence: 99%

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Timing of eclipsing binary V0873 Per: a third body candidate

Bogomazov

Ibrahimov

Satovskii

et al. 2015

Astrophys Space Sci

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We analyse a set of moments of minima of eclipsing variable V0873 Per. V0873 Per is a short period low mass binary star. Data about moments of minima of V0873 Per were taken from literature and our observations during 2013-2014. Our aim is to test the system on existence of new bodies using timing of minima of eclipses. We found the periodical variation of orbital period of V0873 Per. This variation can be explained by the gravitational influence of a third companion on the central binary star. The mass of third body candidate is $\approx 0.2 M_{\odot}$, its orbital period is $\approx 300$ days. The paper also includes a table with moments of minima calculated from our observations which can be used in future investigations of V0873 Per.Comment: 8 pages, 5 figures, 4 tables, accepted for publication in Astrophysics and Space Scienc

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Period change investigation of the low mass ratio contact binary BO Ari

2016

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A photometric study and period change analysis for the A-type low mass ratio contact binary BO Ari is presented. The BV R light curves were fitted by using the Wilson-Devinney method. The photometric solution yields a low mass ratio of q = 0.1754(±0.0016) with a contact degree of f = 27.72%(±2.37%). We found a long-term orbital period decrease at a rate of dP/dt = −3.49 × 10 −7 d yr −1. This result indicates that the system is undergoing mass transfer from the primary component to the secondary with a mass transfer rate ofṁ 1 /m 1 = −7.77 × 10 −8 yr −1. With the period decrease, the inner and outer critical Roche surfaces will tighten and cause the degree of contact to increase. Therefore, BO Ari may evolve into a deeper contact system.

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A photometric study of a weak-contact binary: V873 Per

Cited by 9 publications

References 25 publications

BM UMa: a middle shallow contact binary at pre-transition stage of evolution from W-type to A-type

BM UMa: a middle shallow contact binary at pre-transition stage of evolution from W-type to A-type

Timing of eclipsing binary V0873 Per: a third body candidate

Period change investigation of the low mass ratio contact binary BO Ari

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