V1294 Aql = HD 184279: A bad boy among Be stars or an important clue to the Be phenomenon?. (arXiv:2206.11649v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Harmanec_P/0/1/0/all/0/1">P. Harmanec</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bozic_H/0/1/0/all/0/1">H. Božić</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Koubsky_P/0/1/0/all/0/1">P. Koubský</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yang_S/0/1/0/all/0/1">S. Yang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ruzdjak_D/0/1/0/all/0/1">D. Ruždjak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sudar_D/0/1/0/all/0/1">D. Sudar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Slechta_M/0/1/0/all/0/1">M. Šlechta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wolf_M/0/1/0/all/0/1">M. Wolf</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Korcakova_D/0/1/0/all/0/1">D. Korčáková</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zasche_P/0/1/0/all/0/1">P. Zasche</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Oplistilova_A/0/1/0/all/0/1">A. Oplištilová</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vrsnak_D/0/1/0/all/0/1">D. Vršnak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ak_H/0/1/0/all/0/1">H. Ak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Eenens_P/0/1/0/all/0/1">P. Eenens</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bakis_H/0/1/0/all/0/1">H. Bakiş</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bakis_V/0/1/0/all/0/1">V. Bakiş</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Otero_S/0/1/0/all/0/1">S. Otero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chini_R/0/1/0/all/0/1">R. Chini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Demsky_T/0/1/0/all/0/1">T. Demsky</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barlow_B/0/1/0/all/0/1">B.N. Barlow</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Svoboda_P/0/1/0/all/0/1">P. Svoboda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jonak_J/0/1/0/all/0/1">J. Jonák</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vitovsky_K/0/1/0/all/0/1">K. Vitovský</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Harmanec_A/0/1/0/all/0/1">A. Harmanec</a>
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 25000 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 solar masses. 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.
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 25000 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 solar masses. 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.
http://arxiv.org/icons/sfx.gif
