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The Apsidal Motion of the Eclipsing Binary GSC 4487 0347 = V 957 CEP

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We have made high accuracy CCD observations of the eclipsing binary star GSC 4477 0347 during 2009-2013 and obtained light curves. The photometric parameters and elements of the orbits, and the ephemerides of the primary and secondary minima have been obtained. The longitude angles of the orbital periastron obtained for different observational seasons have been used to calculate the apsidal motion: 𝜔obs = 2.28 ± 0.04° /year. This is a factor of 1.5 faster than the theoretical value calculated for the primary lifetime of the component stars, which are class B8V + B9V on the Main sequence. Either we have actually found the stars within a short segment of their times of entry into the Main sequence or the apsidal motion is affected by the presence of a third body in the system, as indicated by a “third” light in the solution of the light curves ( L3 ≈ 10 % ≈ of the brightness of the entire system).

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Authors and Affiliations

  1. M. V. Lomonosov Moscow State University, P. K. Shternberg State Institute of Astronomy, Moscow, Russia

    V. S. Kozyreva

  2. National Space Agency of Kazakhstan, V. G. Fesenkov Institute of Astronomy, Almaty, Kazakhstan

    A. V. Kusakin

Authors
  1. V. S. Kozyreva
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  2. A. V. Kusakin
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Corresponding authors

Correspondence to V. S. Kozyreva or A. V. Kusakin.

Additional information

Translated from Astrofizika, Vol. 57, No. 2, pp. 237-247 (May 2014).

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Kozyreva, V.S., Kusakin, A.V. The Apsidal Motion of the Eclipsing Binary GSC 4487 0347 = V 957 CEP. Astrophysics 57, 221–230 (2014). https://doi.org/10.1007/s10511-014-9328-7

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  • DOI: https://doi.org/10.1007/s10511-014-9328-7

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