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A Model of the Dust Envelope of the Carbon Mira Star V CrB from Photometry, Infrared Spectroscopy, and Speckle Polarimetry

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Abstract

\(UBVJHKLM\) photometry for the carbon Mira star V CrB are presented. The infrared observations were carried out in the time interval 1989–2018, while the \(U\), \(B\), and \(V\) data were obtained in 2001–2014. The light and color curves are analyzed. The pulsation period of V CrB has been found to be \(355\overset{\textrm{d}}{.}2\) in the infrared \(JHKLM\) bands and \(352^{\textrm{d}}\) for the optical \(BV\) band. In the \(JHK\) bands, apart from periodic pulsations, there are distinct sinusoidal variations in the average brightness level with a characteristic period of \({\sim}8300\) days. Color–magnitude relationships have been revealed for the infrared and optical bands. The phase curves exhibit the wavelength dependence of the brightness variability amplitude. The light curves for various bands and colors are discussed. We have constructed the model of a spherically symmetric circumstellar dust envelope that allows the observed spectral energy distribution at both maximum and minimum light to be reproduced equally well (within the model assumptions) and is consistent with the observations of V CrB by differential speckle polarimetry. The model is characterized by the following parameters: the optical depth is \(\tau_{K}=0.33\), the inner and outer radii of the envelope are 8 and 40 000 AU, respectively. The envelope contains spherical carbon dust grains (\(3/4\) by mass) and silicon carbide dust grains. Dust grains with a radius of 0.5 \(\mu\)m account for \(90\%\) of the envelope mass. The remaining \(10\%\) of the mass is accounted for by finer dust with a grain radius of 0.1 \(\mu\)m. Based on the observational data, we have estimated the bolometric flux from V CrB: \(2.6\times 10^{-7}\) and \(5.1\times 10^{-7}\) erg cm\({}^{-2}\) s\({}^{-1}\) at minimum and maximum light, respectively. The effective temperature of the star is \(T_{\textrm{max}}=3000\) K at maximum light and \(T_{\textrm{min}}=2400\) K at minimum light.

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Funding

The work of A.A. Fedoteva and A.M. Tatarnikov was supported by a grant of the Program for Development of the Moscow State University, the ‘‘Leading Scientific School ‘‘Physics of Stars, Relativistic Objects, and Galaxies’’. B.S. Safonov is grateful to the Russian Science Foundation (project no. 17-12-01241) for supporting the observations by differential speckle polarimetry and their interpretation. The speckle polarimeter was created under financial support by the Program for Development of the Moscow State University.

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Authors and Affiliations

  1. Faculty of Physics, Moscow State University, Moscow, 119991, Russia

    A. A. Fedoteva

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

    A. A. Fedoteva, A. M. Tatarnikov, B. S. Safonov, V. I. Shenavrin & G. V. Komissarova

Authors
  1. A. A. Fedoteva
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  2. A. M. Tatarnikov
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  3. B. S. Safonov
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  4. V. I. Shenavrin
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  5. G. V. Komissarova
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Correspondence to A. A. Fedoteva.

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Translated by V. Astakhov

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Fedoteva, A.A., Tatarnikov, A.M., Safonov, B.S. et al. A Model of the Dust Envelope of the Carbon Mira Star V CrB from Photometry, Infrared Spectroscopy, and Speckle Polarimetry. Astron. Lett. 46, 38–57 (2020). https://doi.org/10.1134/S1063773720010016

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  • DOI: https://doi.org/10.1134/S1063773720010016

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