Observational analysis identifies orbital period and negative superhump behavior in a dwarf nova, suggesting new insights into its outburst activity.
The results of the analysis of photometric observations of the long-period SU UMa-type dwarf nova MASTER OT J212624.16+253827.2 are presented based on the data of ZTF, ATLAS, GAIA, ASAS-SN obtained in 2018–2023 (HJD 245 6772–246 0568) and the Crimean Astrophysical Observatory obtained in 2023–2024 (HJD 246 0199–246 0576) at different stages of outburst activity. We found that this observation interval is notable for variations in the dwarf nova supercycle and cycle, equal to 146–184 days and 12–37 days, respectively. For the first time, we determined the orbital period equal to 0.0865044(2) days, which dominated in the 2018–2023 (HJD 245 8228–245 8836) quiescence and the period of negative superhumps 0.083–0.084 days, which dominated in 2023–2024 (HJD 246 0199–246 0576) quiescence. The estimated mass ratio of the system components is 0.21(2).
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E. P. Pavlenko (2025) studied this question.
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