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.

中文翻译：

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长期侏儒新星V2466 Cyg：2003和2019年爆发

摘要

呈现了不寻常的矮新星V2466 Cygni在其2003年和2019年爆发期间的首次多色光度观测结果。\（R_ {c} \）波段中2019年超爆发的总振幅为7.4个量级。在2019年超级爆发结束时观察到了一次单独的变亮。在分析超级驼峰的\（OC \）图时，我们确定了对应于其周期演变的明显阶段A，B和C。两个超级爆发的平均超级驼峰周期为\（P = 0 \ overset {\ textrm {d}} {。} 08143（3）\）；超驼峰周期导数为\（P _ {\ textrm {dot}} = 10.4（1.4）\ times 10 ^ {-5} \）在阶段B中。我们主张将V2466 Cyg归类为一小群对象的成员，结合SU UMa和WZ Sge矮新星的特征，并提出这些对象的进化状态的解释。另外，我们在V2466 Cyg附近发现并研究了20个新的变星。