Photometric and spectral evolution of the symbiotic eclipsing variable V1329 Cygni at a late stage of its nova-like outburst

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• 作者：V. P. Arkhipova ; V. F. Esipov ; N. P. Ikonnikova ; G. V. Komissarova
• 关键词：symbiotic stars ; UBV observations ; post ; outburst spectral evolution ; phase color curves ; line intensity variations ; colliding winds in binary systems ; V1329 Cyg
• 刊名：Astronomy Letters
• 出版年：2015
• 出版时间：March 2015
• 年：2015
• 卷：41
• 期：3-4
• 页码：128-142
• 全文大小：1,060 KB
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• 作者单位：V. P. Arkhipova (1)
  V. F. Esipov (1)
  N. P. Ikonnikova (1)
  G. V. Komissarova (1)
  
  1. Sternberg Astronomical Institute, Moscow State University (SAI-MSU), Universitetskii pr. 13, Moscow, 119992, Russia
  
• 刊物类别：Physics and Astronomy
• 刊物主题：Physics
  Astronomy
  Astrophysics
  Russian Library of Science
  
• 出版者：MAIK Nauka/Interperiodica distributed exclusively by Springer Science+Business Media LLC.
• ISSN：1562-6873

文摘

The photoelectric UBV observations of the peculiar symbiotic star V1329 Cyg performed at the Crimean Station of the SAI-MSU during 245 nights over the period 2003-014 are presented. The star’s light curves since 1973 from the Crimean observations are shown. The brightness decline after its outburst over the last 40 years was \(0_ \cdot ^m 8 - 1_ \cdot ^m 0\). The phase color curves at phases 0.2 and 0.8 have maxima. Their qualitative interpretation in terms of the model of interacting winds in symbiotic binary star systems is proposed. The orbital period of the binary system has been redetermined. The spectroscopic observations at the 125-cm telescope of the Crimean Station from 1994 to 2014 have confirmed the change in the system’s emission spectrum with orbital phase. The HI, He I, and Fe II line fluxes clearly trace the orbital motion. The Balmer hydrogen lines as well as the continuum at λ6000 and the V-band flux change by a factor of ?.5 from minimum to maximum light. The neutral helium lines change by a factor of 5. The high-excitation He II, [FeVII], [Ca VII] lines and the Raman O VI λ6825 line have shown changes in the fluxes by a factor of ?- weakly correlating with the orbital phase. The equivalent widths of the HI and He I lines are maximal at the star’s maximum light and have distinct minima at phases 0.2 and 0.8, while the equivalent widths of the He II, [FeVII], and [CaVII] lines are minimal in the range of phases 0.2-.8. The question about the location of the permitted and forbidden line emission zones in the binary system V1329 Cyg is discussed. The evolution of the emission spectrum for V1329 Cyg from 1980 to 2014 has been studied on the basis of new and archival data. A gradual decrease in the absolute fluxes of the nebular emission lines has been detected. The [O III] and [Fe VII] lines have weakened significantly. However, the [Fe X] λ6375 ? line has appeared and gradually strengthened, suggesting an increase in the degree of gas ionization in the line formation zone.