Searching for Phase-Locked Variations of the Emission-Line Profiles in Binary Be Stars

Miroshnichenko A.S. Chari R. Danford S. Prendergast P. Aarnio A.N. Andronov I.L. Chinarova L.L. Lytle A. Amantayeva A. Gabitova I.A. Vaidman N.L. Baktybayev S.S. Khokhlov S.A.
August 2023 Multidisciplinary Digital Publishing Institute (MDPI)

Galaxies
2023 #11 Issue 4

There is growing evidence that many Be stars are parts of binary systems. As the B-type primaries are very fast rotators and their spectral lines may be distorted by the circumstellar material, it is not easy to measure their radial velocity directly from the spectral lines. It has been shown that some Be binaries exhibit peak intensity variations consisting of double-peaked H (Formula presented.) lines that are phase-locked with orbital periods. We searched for such variations in the spectra of 12 Be stars, including several known and suspected binaries. Our results include confirmation of the orbital periods in (Formula presented.) Geminorum, (Formula presented.) Capricorni, (Formula presented.) Draconis, 60 Cygni, and V2119 Cygni, its refinement in o Puppis, as well as suggesting hints for binarity in o Aquarii, BK Camelopardalis, and 10 Cassiopeae. Monitoring of the H (Formula presented.) line profile variations in (Formula presented.) Canis Minoris for over the last 10 years gives further support to the existence of a 182.5-day period found earlier in a smaller set of data. A similar but still preliminary period (179.6 days) was found in the H (Formula presented.) line profile variations in (Formula presented.) Persei. It is shown for the first time that (Formula presented.) Geminorum exhibits phase-locked variations in the H (Formula presented.) emission peak intensity ratio and, therefore, is a part of the inner binary in this triple system. Our results show that the mentioned phase-locked peak intensity variations are observed in more Be binary systems than previously known and can be used to search for binarity of Be stars when application of other methods is inconclusive.

binary system , circumstellar matter , data analysis , emission-line stars , spectroscopy , variable stars

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Department of Physics and Astronomy, University of North Carolina—Greensboro, Greensboro, 27402, NC, United States
Fesenkov Astrophysical Institute, Observatory, 23, Almaty, 050020, Kazakhstan
Department of Physics and Astronomy, University of Tennessee, Knoxville, 37996, TN, United States
Kernersville Observatory, Winston-Salem, 27285, NC, United States
Department of Mathematics, Physics and Astronomy, Odesa National Maritime University, Mechnikova St. 34, Odesa, 65029, Ukraine
Faculty of Physics and Technology, Al-Farabi Kazakh National University, Al-Farabi Ave., 71, Almaty, 050040, Kazakhstan

Department of Physics and Astronomy
Fesenkov Astrophysical Institute
Department of Physics and Astronomy
Kernersville Observatory
Department of Mathematics
Faculty of Physics and Technology

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