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B[e] Star CI Camelopardalis in the Optical Range

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Abstract

We report the results of photometric and spectroscopic monitoring of CI Cam within 24 years since its outburst in 1998. Over this time, we found a system component emitting in the He II 4686 Å emission line, on an elliptical orbit with a period of \(19\overset{\textrm{d}}{.}407\) days and an eccentricity of 0.44–0.49. The variations of the optical brightness are observed with the same period and with an average amplitude of \(0\overset{\textrm{m}}{.}04\). The total amplitude of the He II radial velocity variations is about 380 km s\({}^{-1}\). The equivalent width of the line is variable on a time scale of tens of minutes as well as with the orbital period. Maximum equivalent widths of the He II line are observed when the component passes the descending node of the orbit. The intensity of the He II 4686 Å emission gradually increases with time. Slow radial velocity variations on a scale of decades were detected by means of high resolution spectroscopy in the iron emission lines and a forbidden nitrogen line formed in the circumstellar nebula. The B-type star turned out to be a pulsating variable. During the period between 2005 and 2009, pulsations were multiperiodic with the dominant periods \(0\overset{\textrm{d}}{.}5223\), \(0\overset{\textrm{d}}{.}41539\), and \(0\overset{\textrm{d}}{.}26630\) days. However, since 2012 it has pulsated in a single mode with a variable period in the \(0\overset{\textrm{d}}{.}403{-}0\overset{\textrm{d}}{.}408\) day range depending on the star’s luminosity. We identify the 2005–2009 pulsations as a resonance of the radial modes, and the residual stable mode as the first overtone. The pulsations are coherent on a scale of several months, and their average amplitudes are \(0\overset{\textrm{m}}{.}02{-}0\overset{\textrm{m}}{.}04\). The pulsation data constrain the spectral type of the main component to B0–B2 III, the distance to the system to 2.5–4.5 kpc, and the absolute visual magnitude \(M_{V}\) to the range of \(-3\overset{\textrm{m}}{.}7\) to \(-4\overset{\textrm{m}}{.}9\). The classification of the CI Cam main component as a B[e] supergiant is completely ruled out due to the observed pulsation periods. CI Cam may be a system at the stage after the first mass exchange and may be attributed to the FS CMa-type group of objects with the B[e] phenomenon.

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Notes

  1. Developed by V. P. Goranskij.

  2. https://outerspace.stsci.edu/display/TESS/TESS+Holdings+Available+by+MAST+Service

  3. Developed by V.P. Goranskij.

  4. Slowly Pulsating B-stars.

  5. SLF—a stochastic low-frequency process—random, unpredictable light variations which can be described by one mathematical parameter.

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ACKNOWLEDGMENTS

The authors are grateful to N.V. Borisov, A.F. Valeev, G.G. Valyavin, A.S. Vinokurov, V.V. Vlasyuk, V.G. Klochkova, D.N. Monin, V.E. Panchuk, S.N. Fabrika, M.V. Yushkin and S.Yu. Shugarov, who took part in the observations, showed an interest in this investigation, and provided observational material for analysis.

This work makes use of the Gaia DR1–DR3 databases, TESS (Mikulski Archive for Space Telescopes at STScI), and the NIST Atomic Spectra Database.

Observations with the SAO RAS telescopes are supported by the Ministry of Science and Higher Education of the Russian Federation. The renovation of telescope equipment is currently provided within the national project ‘‘Science and Universities’’. The work was performed as part of the SAO RAS government contract approved by the Ministry of Science and Higher Education of the Russian Federation.

We thank the Russian Telescope Time Allocation Committee for providing the BTA observing time, and also the administration of SAO RAS for the Zeiss-1000 telescope observing time.

V.P. Goranskij and E.A. Barsukova are grateful to the administrations of MSU, SAI and the Crimean Astronomical Station of SAI MSU for the alloted Crimean station telescope time and longstanding support of the work on this subject.

This paper is partly based on observations obtained at the Canada-France-Hawaii Telescope (CFHT), which is operated by the National Research Council of Canada, the Institute National des Sciences de l’Univers of the Centre National de la Recherche Scientifique de France, and the University of Hawaii. The observations at CFHT were performed with care and respect from the summit of Maunakea, which is a significant cultural and historic site.

Funding

P.L.N., L.H.I. and K.A.S. would like to thank the Bulgarian Research Foundation for partial financial support of this work with a bilateral grant KP-06-RUSSIA-9/2019. The study was financially supported by the Russian Foundation for Basic Research and the National Science Foundation of Bulgaria as a part of the scientific project No. 19-52-18007 and Grant KP-06-Russia-9/2019. S.Z. and A.M. acknowledge PAPIIT grants IN102120 and IN119323. This research has been funded in part by the Science Committee of the Ministry of Education and Science of the Republic of Kazakhstan (Grant No. AP08856419).

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Authors and Affiliations

  1. Special Astrophysical Observatory, Russian Academy of Sciences, 369167, Nizhnii Arkhyz, Russia

    E. A. Barsukova, A. N. Burenkov, V. P. Goranskij, A. V. Moiseeva, E. A. Semenko & I. A. Yakunin

  2. Sternberg Astronomical Institute, Moscow State University, 119234, Moscow, Russia

    V. P. Goranskij & N. V. Metlova

  3. Institute of Astronomy, National Autonomous University of Mexico, 22800, Ensenada, Baja California, Mexico

    S. V. Zharikov

  4. Al-Farabi Kazakh National University, 050040, Almaty, Kazakhstan

    S. V. Zharikov & A. S. Miroshnichenko

  5. Institute of Astronomy and National Astronomical Observatory Rozhen, Bulgarian Academy of Sciences, 1784, Sofia, Bulgaria

    L. Iliev & K. Stoyanov

  6. Canadian-French-Hawaiian Telescope Corporation (CFHT), 96743, Kamuela, Hawaii, USA

    N. Manset

  7. University of North Carolina at Greensboro, 27402, Greensboro, USA

    A. S. Miroshnichenko

  8. Central (Pulkovo) Astronomical Observatory, Russian Academy of Sciences, 196140, St. Petersburg, Russia

    A. S. Miroshnichenko

  9. Fesenkov Astronomical Institute, 050020, Almaty, Kazakhstan

    A. S. Miroshnichenko

  10. Department of Astronomy, Sofia University, 1504, Sofia, Bulgaria

    P. L. Nedialkov

  11. National Astronomical Research Institute of Thailand, 50180, Mae Rim, Chiang Mai, Thailand

    E. A. Semenko

  12. St. Petersburg University, 199034, St. Petersburg, Russia

    I. A. Yakunin

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  1. E. A. Barsukova
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  2. A. N. Burenkov
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  3. V. P. Goranskij
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  5. L. Iliev
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  6. N. Manset
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  7. N. V. Metlova
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  8. A. S. Miroshnichenko
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  9. A. V. Moiseeva
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  13. I. A. Yakunin
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Correspondence to E. A. Barsukova.

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Translated by L. Chmyreva

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Barsukova, E.A., Burenkov, A.N., Goranskij, V.P. et al. B[e] Star CI Camelopardalis in the Optical Range. Astrophys. Bull. 78, 1–24 (2023). https://doi.org/10.1134/S1990341323010029

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