Kinematics and Physics of Celestial Bodies

, Volume 33, Issue 5, pp 231–238 | Cite as

Investigation of the lines Hα and Hβ in the spectrum of the star HD 206267

Physics of Stars and Interstellar Medium


The results of investigations of the Hα and Hβ lines in the spectrum of the star HD 206267 are presented. Observations were carried out in 2011–2014 at the Cassegrain focus of the 2-m telescope of the Tusi Shamakhy Astrophysical Observatory of the National Academy of Sciences of Azerbaijan using an echelle spectrometer. The following features have been revealed for the first time: the moving discrete absorption components in the core of the Hα line from the red side to the violet, the stable emission in the violet wing of the Hα line, the antiphase variation of the radial velocities and equivalent widths of the Hα line, and the independence of the changes of the equivalent widths of the Hβ line from the phase of the orbital period. No spectral features according to which this star could be considered as a source of X-ray radiation have been found.


Unable to display preview. Download preview PDF.

Unable to display preview. Download preview PDF.


  1. 1.
    G. A. Galazutdinov, Preprint No. 92, SAO RAN (Special Astrophysics Observatory of the Russian Academy of Sciences, Nizhny Arkhyz, 1992).Google Scholar
  2. 2.
    T. S. Galkina, “Spectral Observations of HD 206267, identified with X-ray source Ser X-4,” Izv. Krym. Astrofiz. Obs. 63, 86–92 (1981).ADSGoogle Scholar
  3. 3.
    A. G. Masevich and A. V. Tutukov, Stellar Evolution: Theory and Observations (Nauka, Moscow, 1988) [in Russian].Google Scholar
  4. 4.
    X. M. Mikhailov, V. M. Khalilov, and I. A. Alekberov, “Echelle-spectrophotometer of Cassegrain focus of the 2-meter telescope at Shamakhi Astrophysical Observatory,” Tsirk. Shemakhin. Astrofiz. Obs. Nats. Akad. Nauk Az. 109, 21–30 (2005).Google Scholar
  5. 5.
    D. K. Rustamov and A. F. Abdulkerimova, “Asymmetry of the interstellar lines Na I λ 589.0 and 589.6 nm in the spectrum of the Wolf–Rayet type star HD 192163,” Kinematics Phys. Celestial Bodies 31, 100–104 (2015).ADSCrossRefGoogle Scholar
  6. 6.
    D. N. Rustamov and A. M. Cherepashchuk, “The Wolf–Rayet star HD 192163 as a possible evolutionary progenitor of a low-mass X-ray binary,” Astron. Rep. 55, 347–358 (2011).ADSCrossRefGoogle Scholar
  7. 7.
    D. N. Rustamov and A. M. Cherepashchuk, “Spectral and photometric studies of the Wolf–Rayet star WR 134 = HD 191765,” Astron. Rep. 56, 761–774 (2012).ADSCrossRefGoogle Scholar
  8. 8.
    H. A. Abt, “The ages and dimensions of Trapezium systems,” Astrophys. J. 304, 688–694 (1986).ADSCrossRefGoogle Scholar
  9. 9.
    D. Crampton and R. O. D. Redman, “Binary O star HR 8281,” Astron. J. 80, 454–457 (1975).ADSCrossRefGoogle Scholar
  10. 10.
    J. A. Harvin, “Doppler tomography of massive compact binary stars in multiple star systems,” Bull. Am. Astron. Soc. 33, 1532 (2001).ADSGoogle Scholar
  11. 11.
    J. A. Harvin, “Doppler tomography of the massive compact binary stars in the multiple star systems d Orionis and HD 206267,” Publ. Astron. Soc. Pac. 116, 186–186 (2004).ADSCrossRefGoogle Scholar
  12. 12.
    J. A. Harvin, D. R. Gies, and L. R. Penny, “The components of the HD 206267 A triple star system,” Bull. Am. Astron. Soc. 35, 1223 (2003).ADSGoogle Scholar
  13. 13.
    G. Hensberge and R. H. Hammerschlag, “HD 206267, a candidate star for the transient X-ray source Cepheus X-4?,” Astron. Astrophys. 39, 157–158 (1975).ADSGoogle Scholar
  14. 14.
    L. Kaper, H. F. Henrichs, J. S. Nichols, and J. H. Telting, “Long-and short-term variability in O-star winds. II. Quantitative analysis of DAC behaviour,” Astron. Astrophys. 344, 231–262 (1999).ADSGoogle Scholar
  15. 15.
    A. Kaufer, O. Stahl, V. Wolf, Th. Gang, A. Gummersbach S, J. Kovacs, H. Mandel, and Th. Szeifert, “Longterm spectroscopic monitoring of BA-type supergiants. I. Ha line-profile variability,” Astron. Astrophys. 305, 887–901 (1996).ADSGoogle Scholar
  16. 16.
    A. Lobel and R. Blomme, “Modeling ultraviolet wind line variability in massive hot stars,” Astrophys. J. 678, 408–430 (2008).ADSCrossRefGoogle Scholar
  17. 17.
    N. Markova, “New aspects of line-profile variability in P Cygni’s optical spectrum,” Astron. Astrophys. Suppl. Ser. 144, 391–404 (2000).ADSCrossRefGoogle Scholar
  18. 18.
    R. K. Prinja, M. J. Barlow, and I. D. Howarth, “Terminal velocities for a large sample of O stars. V supergiants, and Wolf–Rayet stars,” Astrophys. J. 361, 607–620 (1990).ADSCrossRefGoogle Scholar
  19. 19.
    J. T. Puis, J. S. Vink, and F. Najarro, “Mass loss from hot massive stars,” Astron. Astrophys. Rev. 16, 209–325 (2008).ADSCrossRefGoogle Scholar
  20. 20.
    W. C. Rufus, “The variable radial velocity of the star, BD+56[degrees]2617(A),” Publ. Obs. Univ. Mich. 6, 45–47 (1937).ADSGoogle Scholar
  21. 21.
    D. J. Stickland, “Spectroscopic binary orbits from ultraviolet radial velocities. Paper 17: HD 206267,” Observatory 115, 180–185 (1995).ADSGoogle Scholar
  22. 22.
    M. P. Ulmer, W. A. Baity, W. A. Wheaton, and L. E. Peterson, “New transient source, Cepheus X-4, observed by OSO-7,” Astrophys. J. Lett. 184, L117–L120 (1973).ADSCrossRefGoogle Scholar
  23. 23.
    W. L. Waldron and J. P. Cassinelli, “An extensive collection of stellar wind X-Ray source region emission line parameters, temperatures, velocities, and their radial distributions as obtained from Chandra observations of 17 OB stars,” Astrophys. J. 668, 456–480 (2007).ADSCrossRefGoogle Scholar
  24. 24.
    P. S. Wojdowski, N. S. Schulz, K. Ishibashi, and D. P. Huenemoerder, “The hot star triplet HD 206267A,” in High Resolution X-ray Spectroscopy with XMM-Newton and Chandra: Proc. Int. Workshop, Holmbury St Mary, UK, Oct. 24–25, 2002, Ed. by G. Branduardi-Raymont, pp. 1–4.Google Scholar

Copyright information

© Allerton Press, Inc. 2017

Authors and Affiliations

  1. 1.Tusi Shamakhy Astrophysical ObservatoryNational Academy of Sciences of AzerbaijanBakuAzerbaijan

Personalised recommendations