Abstract
We present the results of our photometric (V RI) and spectroscopic observations of the young variable star V730 Cep (MisV1147) classified by Uemura et al. (2004) as a Herbig Be star. Our photometry confirms the conclusion of the above authors that this star has a complex pattern of variability including periodic or quasi-periodic brightness variations with a period of about 14 days and deep Algol-like minima typical for UX Ori stars. Our spectroscopy shows that the classification of V730 Cep as a Herbig Be star is wrong. Actually, this star has a much lower temperature and belongs to the family of T Tauri stars. This allows us to explain the nature of the unusual photometric activity of V730 Cep based on a combination of two well-known models of variable circumstellar extinction applied to young stars: AA Tau- and UX Oritype variability. It follows from our observations that the color tracks on the V −(V −I) color–magnitude diagram for these models slightly differ: the AA Tau-type variability of circumstellar extinction is caused by larger grains than the UX Ori-type variability. Such a difference can be due to an increase in the characteristic sizes of circumstellar dust as the star is approached and has a simple explanation: small dust grains evaporate faster than large ones.
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Original Russian Text © V.P. Grinin, K.A. Antonyuk, I.S. Potravnov, D. Mkrtichian, 2018, published in Pis’ma v Astronomicheskii Zhurnal, 2018, Vol. 44, No. 12, pp. 868–873.
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Grinin, V.P., Antonyuk, K.A., Potravnov, I.S. et al. Results of Photometric and Spectroscopic Observations of the Young Variable Star V730 Cep. Astron. Lett. 44, 798–802 (2018). https://doi.org/10.1134/S1063773718120022
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DOI: https://doi.org/10.1134/S1063773718120022