2025/12/06 by Tarasenkov, Alexander, Shugarov, Sergey, Ikonnikova, Natalia +3
#FOS: Physical sciences #Solar and Stellar Astrophysics (astro-ph.SR)
paper · doi:10.48550/arxiv.2512.06372
We present the results of photometric analysis of WZ Sge type dwarf nova TCP J20171288+1156589. This object exhibited an outburst with a large amplitude of >7.9 magnitudes and was observed for over a month. The photometric evolution of the superoutburst was atypical for WZ Sge-type dwarf novae. Periodogram analisys reveals early superhumps with the most probable period of 0.0611±0.0001 days during the initial decline. After a plateau phase of approximately 11 days, ordinary superhumps (likely stage B) emerged with a period of 0.0616±0.0001 days, corresponding to a superhump excess of ε=0.008 correspondingly. This delay in the onset of ordinary superhumps is an unusual feature among WZ Sge stars. We evaluated the main parameters of the system: mass ratio q=MRD/MWD=0.06±0.005, yielding component masses of MWD∼1.0±0.15M\odot for the white dwarf and MRD=0.06±0.01M\odot for the donor. The estimated distance to the system is ∼850 pc, and the binary separation is a=0.67±0.03R\odot.