V1294 Aql = HD 184279: A bad boy among Be stars or an important clue to the Be phenomenon?

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Harmanec P., Božić H., Koubský P., Yang S., Ruždjak D., Sudar D., ...Daha Fazla

Astronomy and Astrophysics, cilt.666, 2022 (SCI-Expanded) identifier identifier identifier

  • Yayın Türü: Makale / Tam Makale
  • Cilt numarası: 666
  • Basım Tarihi: 2022
  • Doi Numarası: 10.1051/0004-6361/202244006
  • Dergi Adı: Astronomy and Astrophysics
  • Derginin Tarandığı İndeksler: Science Citation Index Expanded (SCI-EXPANDED), Scopus, Academic Search Premier, Aerospace Database, Artic & Antarctic Regions, Communication Abstracts, Compendex, INSPEC, Metadex, zbMATH, DIALNET, Civil Engineering Abstracts
  • Anahtar Kelimeler: binaries: spectroscopic, stars: emission-line, Be, stars: fundamental parameters, MIDTERM SPECTROSCOPIC VARIATIONS, LONG-TERM, SHELL STARS, ORBITAL ELEMENTS, V/R VARIATIONS, BINARY, VARIABILITY, DISK, SPECTROGRAPH, MAGNITUDES
  • Kayseri Üniversitesi Adresli: Hayır

Özet

© 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.