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Periodic variability of the T tauri star DI cephei

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Abstract

Original spectroscopic and photometric observations are used together with data from the literature to compile a master light curve for DI Cep and to analyze individual data series for periodicity. The spectroscopic data reveal the period P=9.24d. Data from different authors show the nine-day quasi-periodicity in the brightness variations fairly reliably, although the period cannot be derived from the entire master set of photometric data. The period P=18.28d is also derived from the V brightnesses. We find variations of the zero epoch of the nine-day period, possibly due to the changing location of an accretion-disk hot spot.

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Authors and Affiliations

  1. Shemakha Astrophysical Observatory, National Academy of Sciences of Azerbaijan, Shemakha, 373243, Azerbaijan

    N. Z. Ismailov

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  1. N. Z. Ismailov
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Translated from Astronomicheski\(\overset{\lower0.5em\hbox{$\smash{\scriptscriptstyle\smile}$}}{l} \) Zhurnal, Vol. 81, No. 5, 2004, pp. 431–437.

Original Russian Text Copyright © 2004 by Ismailov.

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Ismailov, N.Z. Periodic variability of the T tauri star DI cephei. Astron. Rep. 48, 393–398 (2004). https://doi.org/10.1134/1.1744939

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