| Issue |
A&A
Volume 666, October 2022
|
|
|---|---|---|
| Article Number | A136 | |
| Number of page(s) | 15 | |
| Section | Stellar structure and evolution | |
| DOI | https://doi.org/10.1051/0004-6361/202244006 | |
| Published online | 17 October 2022 | |
V1294 Aql = HD 184279: A bad boy among Be stars or an important clue to the Be phenomenon?⋆,⋆⋆
1
Astronomical Institute of Charles University, Faculty of Mathematics and Physics, V Holešovičkách 2, 180 00 Praha 8, Troja, Czech Republic
e-mail: Petr.Harmanec@mff.cuni.cz
2
Hvar Observatory, Faculty of Geodesy, University of Zagreb, Kačićeva 26, 10000 Zagreb, Croatia
3
Astronomical Institute, Czech Academy of Sciences, 251 65 Ondřejov, Czech Republic
4
Physics & Astronomy Department, University of Victoria, PO Box 3055 STN CSC, Victoria, BC V8W 3P6, Canada
5
Faculty of Electrical Engineering and Computing, University of Zagreb, Unska 3, 10000 Zagreb, Croatia
6
Astronomy and Space Sci. Dept., Science Faculty, Erciyes University, 38039 Kayseri, Turkey
7
Dept. of Astronomy, University of Guanajuato, 36000 Guanajuato, GTO, Mexico
8
Dept. of Space Sciences and Technology, Akdeniz University, 07058 Antalya, Turkey
9
Buenos Aires, Argentina and American Association of Variable Star Observers (AAVSO), 49 Bay State Road, Cambridge, MA 02138, USA
10
Astronomisches Institut, Ruhr–Universität Bochum, Universitätsstr. 150, 44801 Bochum, Germany
11
Instituto de Astronomía, Universidad Católica del Norte, Avenida Angamos 0610, Casilla 1280 Antofagasta, Chile
12
Department of Physics, High Point University, One University Way, High Point, NC 27268, USA
13
Private Observatory, Vypustky 5, Brno 614 00, Czech Republic
14
Faculty of Mathematics and Physics, Charles University, Prague, Czech Republic
Received:
12
May
2022
Accepted:
9
June
2022
A reliable determination of the basic physical properties and variability patterns of hot emission-line stars is important for understanding the Be phenomenon and ultimately, the evolutionary stage of Be stars. This study is devoted to one of the most remarkable Be stars, V1294 Aql = HD 184279. We collected and analysed spectroscopic and photometric observations covering a time interval of about 25 000 d (68 yr). We present evidence that the object is a single-line 192.9 d spectroscopic binary and estimate that the secondary probably is a hot compact object with a mass of about 1.1–1.2 M⊙. We found and documented very complicated orbital and long-term spectral, light, and colour variations, which must arise from a combination of several distinct variability patterns. Attempts at modelling them are planned for a follow-up study. We place the time behaviour of V1294 Aql into context with variations known for some other systematically studied Be stars and discuss the current ideas about the nature of the Be phenomenon.
Key words: binaries: spectroscopic / stars: emission-line, Be / stars: fundamental parameters
Tables 3–5 are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/666/A136
Based on new spectroscopic observations from the ESO FEROS echelle spectrograph; CCD coudé spectrograph of the Astronomical Institute of Czech Academy of Sciences in Ondřejov; CCD coudé spectrograph of the Dominion Astrophysical Observatory; echelle BESO spectrograph of the Universitätssternwarte Bochum; CCD spectrographs of Castanet-Tolosan Observatory; CHIRON echelle spectrograph of Cerro Tololo Observatory; and amateur spectra from the BeSS database, and on photometric observations from Hvar, Toronto, San Pedro Mártir, Tubitak and Çanakkale Observatories, and Hp photometry from the ESA Hipparcos mission.
© P. Harmanec et al. 2022
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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