Photometric and Spectroscopic Study of the Supergiant with an Infrared Excess V1027 Cygni

Arkhipova, V.P.; Taranova, O.G.; Ikonnikova, N.P.; Esipov, V.F.; Komissarova, G.V.; Shenavrin, V.I.; Burlak, M.A.

Авторы: Arkhipova V.P., Taranova O.G., Ikonnikova N.P., Esipov V.F., Komissarova G.V., Shenavrin V.I., Burlak M.A.
Журнал: Astronomy Letters
Том: 42
Номер: 11
Год издания: 2016
Издательство: Maik Nauka/Interperiodica Publishing
Местоположение издательства: Russian Federation
Первая страница: 756
Последняя страница: 773
DOI: 10.1134/S1063773716100017
Аннотация: We present the results of our UBV and JHKLM photometry for the semiregular pulsating variable V1027 Cyg, a supergiant with an infrared excess, over the period from 1997 to 2015 (UBV) and in 2009–2015 (JHKLM). Together with the new data, we analyze the photometric observations of V1027 Cyg that we have obtained and published previously. Our search for a periodicity in the UBV brightness variations has led to several periods from P = 212d to 320d in different time intervals. We have found the period P = 237d based on our infrared photometry. The variability amplitude, the lightcurve shape, and themagnitude of V1027 Cyg atmaximum light change noticeably from cycle to cycle. The deepest minimum was observed in 2011, when the amplitudes of brightness variations in the star reached the following values: ΔU = 1m. 28, ΔB = 1m. 10, ΔV = 1m. 05, ΔJ = 0m. 30, ΔH = 0m. 35, ΔK = 0m. 32, ΔL = 0m. 26, and ΔM = 0m. 10. An ambiguous correlation of the B − V and U − B colors with the brightness has been revealed. For example, a noticeable bluing of the star was observed during the deep 1992, 2008, and 2011 minima, while the variations with smaller amplitudes show an increase in B − V at the photometric minima. The spectral energy distribution for V1027 Cyg from our photometry in the range 0.36 (U)–5.0 (M) μm corresponds to spectral types from G8I to K3I at different phases of the pulsation cycle. Low-resolution spectra of V1027 Cyg in the range λ4400–9200 ˚A were taken during 16 nights over the period 1995–2015. At the 1995 and 2011 photometric minima the star’s spectrum exhibited molecular TiO bands whose intensity corresponded to spectral types M0–M1, while the photometric data point to a considerably earlier spectral type. We hypothesize that the TiO bands are formed in the upper layers of the extended stellar atmosphere. We have measured the equivalent widths of the strongest absorption lines, in particular, the infrared Ca II triplet in the spectrum of V1027 Cyg. The calcium triplet (Ca T) with Wλ(Ca T) = 20.3 ± 1.8 ˚A as a luminosity indicator for supergiants places V1027 Cyg in the region of the brightest G–K supergiants. V1027 Cyg has been identified with the infrared source IRAS 20004+2955 and is currently believed to be a candidate for post-AGB stars. The evolutionary status of the star and its difference from other post-AGB objects are discussed.
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Photometric and Spectroscopic Study of the Supergiant with an Infrared Excess V1027 Cygniстатья

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