Abstract
Results of the first multicolor photometric observations of the unusual dwarf nova V2466 Cygni during its 2003 and 2019 superoutbursts are presented. The total amplitude of the 2019 superoutburst in the \(R_{c}\) band is 7.4 magnitudes. A single rebrightening was observed at the end of the 2019 superoutburst. While analyzing the \(O-C\) diagram for the superhumps, we identified pronounced stages A, B, and C corresponding to the evolution of their period. The mean superhump period is \(P=0\overset{\textrm{d}}{.}08143(3)\) for both superoutbursts; the superhump period derivative is \(P_{\textrm{dot}}=10.4(1.4)\times 10^{-5}\) in stage B. We argue for the classification of V2466 Cyg as a member of a small group of objects combining the characteristics of SU UMa and WZ Sge dwarf novae and propose an explanation for the evolutionary status of these objects. As an additional result, we have discovered and studied 20 new variable stars in the neighborhoods of V2466 Cyg.
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According to the classification of the General Catalogue of Variable Stars (Samus’ et al. 2017), WZ Sge stars are a subclass of SU UMa stars. Following Downes et al. (2001), VSX AAVSO defines them as two separate types of dwarf novae: UGSU and UGWZ.
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ACKNOWLEDGMENTS
We thank Professor K.A. Postnov and Professor N.N. Samus’ for the useful discussions and the anonymous referees for the valuable remarks.
Funding
This study became possible owing to the observations at the 60-cm CMO SAI MSU telescope funded by M.V. Lomonosov Moscow State University Program of Development and owing to the use of the AAVSO Photometric All-Sky Survey (APASS) funded by the Robert Martin Ayers Sciences Fund and NSF AST-1412587. K.V. Sokolovsky thanks the Packard Fund for its support.
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Antipin, S.V., Zubareva, A.M., Belinski, A.A. et al. The Long-Period Dwarf Nova V2466 Cyg: The 2003 and 2019 Superoutbursts. Astron. Lett. 46, 677–690 (2020). https://doi.org/10.1134/S1063773720100011
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DOI: https://doi.org/10.1134/S1063773720100011