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Timing of eclipsing binary V0873 Per: a third body candidate

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Abstract

We analyze 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 the 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 a periodic 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 the third body candidate is \(\approx 0.2~M_{\odot}\), and its orbital period is \(\approx300~\mbox{days}\). The paper also includes a table with moments of minima calculated from our observations, which can be used in future investigations of V0873 Per.

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Notes

  1. V0873 Per = TYC 2853-18-1.

  2. See also General Catalogue of Variable Stars (Samus et al. 2014).

  3. http://c-munipack.sourceforge.net.

  4. We do not use the moment of minimum 2451370.8753 (Nicholson and Varley 2006) following Kriwattanawong and Poojon (2015).

  5. See Kozyreva and Zakharov (2001) for more details. A very similar program was described and used by Khaliullina and Khaliullin (1984).

  6. See Eq. (3) in Kozyreva et al. (2005); also, see Martynov (1948), Kozyreva and Khaliullin (1999), Kozyreva et al. (2005) reported about discoveries of third bodies in AS Cam and HP Aur binaries correspondingly using this method. Lacy et al. (2014) independently confirmed existence of a third body in HP Aur system.

  7. Because their mean square-error is greater than \(2.5\sigma\). We cannot 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.

  8. Orbital period of the new body is \(\approx300~\mbox{days}\), whereas the orbital period of V0873 Per is less than \(0.3~\mbox{days}\). At the same time, a third body is able to possess almost stable orbit if its orbital period begins from \(\approx3~\mbox{days}\); see Table 6 in Holman and Wiegert (1999). So, we can apply Kepler’s third law for such a body (for rough estimations because there should exist strong disturbances of the orbit).

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Acknowledgements

We thank S.Yu. Shugarov, B.M. Shustov, and A.M. Tatarnikov for their kind help in building our team. We are grateful to anonymous referees for very useful comments.

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Authors and Affiliations

  1. Sternberg Astronomical Institute, M.V. Lomonosov Moscow State University, 13, Universitetskii prospect, Moscow, 119991, Russia

    A. I. Bogomazov, V. S. Kozyreva & T. R. Irsmambetova

  2. Institute of Astronomy, Russian Academy of Sciences, 48, Pyatnitskaya ulitsa, Moscow, 119017, Russia

    M. A. Ibrahimov & A. V. Tutukov

  3. AstroTel Ltd., 1A, Nizhegorodskaya ulitsa, Moscow, 109147, Russia

    B. L. Satovskii

  4. Main Astronomical Observatory, National Academy of Sciences of Ukraine, 27, Akademika Zabolotnoho ulitsa, Kyiv, 03680, Ukraine

    V. N. Krushevska & Y. G. Kuznyetsova

  5. Ulugh Beg Astronomical Institute, Uzbek Academy of Sciences, 33, Astronomicheskaya ulitsa, Tashkent, 100052, Uzbekistan

    E. R. Gaynullina, R. G. Karimov & S. A. Ehgamberdiev

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  1. A. I. Bogomazov
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  2. M. A. Ibrahimov
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  3. B. L. Satovskii
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  4. V. S. Kozyreva
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  5. T. R. Irsmambetova
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  6. V. N. Krushevska
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  7. Y. G. Kuznyetsova
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  8. E. R. Gaynullina
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  9. R. G. Karimov
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  10. S. A. Ehgamberdiev
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  11. A. V. Tutukov
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Correspondence to A. I. Bogomazov.

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Bogomazov, A.I., Ibrahimov, M.A., Satovskii, B.L. et al. Timing of eclipsing binary V0873 Per: a third body candidate. Astrophys Space Sci 361, 4 (2016). https://doi.org/10.1007/s10509-015-2591-1

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  • DOI: https://doi.org/10.1007/s10509-015-2591-1

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