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Infrared variability of three hot stars on a time scale of 10–20 years

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Abstract

Long-term (1994–2014) near-infrared observations of P Cyg, kDra, and BUTau are analyzed. It is shown that the observed brightness and color variations in P Cyg and k Dra can be explained by variations in the parameters of the stars themselves and their ionized circumstellar shells, whose excitation requires from 5 to 15% of the star’s luminosity. The emission from BU Tau in the range 1.25–3.5 µm mimics blackbody radiation, and its variability is a consequence of variations in the star’s temperature and, as a result, its radius and luminosity. No excess emission from BU Tau that could be associated with an additional source has been detected.

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Authors and Affiliations

  1. Sternberg Astronomical Institute, Moscow State University, Universitetskii pr. 13, Moscow, 119992, Russia

    O. G. Taranova & V. I. Shenavrin

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  1. O. G. Taranova
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  2. V. I. Shenavrin
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Correspondence to O. G. Taranova.

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Original Russian Text © O.G. Taranova, V.I. Shenavrin, 2015, published in Pis’ma v Astronomicheskiĭ Zhurnal, 2015, Vol. 41, Nos. 3–4, pp. 163–176.

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Taranova, O.G., Shenavrin, V.I. Infrared variability of three hot stars on a time scale of 10–20 years. Astron. Lett. 41, 143–155 (2015). https://doi.org/10.1134/S1063773715040076

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