Abstract
We refined the orbital period of the Herbig Be binary star HD200775 using both new and archive observed data which has been obtained with high-resolution spectrometers at optical wavelengths over 20 years. The new spectroscopic observations were performed with the 1.2-m telescope of the Kourovka Astronomical Observatory of Ural Federal University during 2012–2014 and the 6-m BTA telescope of the Special Astrophysical Observatory in 2013.We show that the period of these observations has a new maximum of activity in 2012 and the following transition of the star to the quiescent state. We confirmed that activity maxima of HD200775, which are characterized by the increase of the Hα equivalent width, appear at intervals of about 3.7 years. A stable orbital period of the system of \(1361_.^d 3 \pm 2_.^d 2\) days was found from radial velocity variations obtained for the He I 5876 Å line. It is shown that the radial velocities determined from the Hα emission line and the He I 5876 Å absorption line, which is formed in the photosphere of the more massive primary component of the system, are close and change synchronously with time. This synchronization indicates the fact that the major portion of the HD200775 Ha emission originates in the material associated with the more massive component of the system.
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Original Russian Text © A.P. Bisyarina, A.M. Sobolev, S.Yu. Gorda, S.Yu. Parfenov, 2015, published in Astrofizicheskii Byulleten, 2015, Vol. 70, No. 3, pp. 316–327.
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Bisyarina, A.P., Sobolev, A.M., Gorda, S.Y. et al. Optical spectroscopic monitoring of the Herbig Be binary star HD 200775: New maximum of activity and refinement of the orbital period. Astrophys. Bull. 70, 299–309 (2015). https://doi.org/10.1134/S1990341315030074
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DOI: https://doi.org/10.1134/S1990341315030074