2009 Superoutburst of Dwarf Nova 1RXS J053234.9+624755

TL;DR

This paper presents detailed photometric analysis of the 2009 superoutburst of dwarf nova 1RXS J053234.9+624755, revealing superhump period evolution, disc dynamics, and quasi-periodic oscillations, contributing to understanding accretion processes in dwarf novae.

Contribution

It provides the first detailed analysis of superhump period changes, disc motion, and oscillations during a superoutburst of this specific dwarf nova, supporting models of superhump origin near the hot spot.

Findings

Superhump period P_sh=0.057122 days.

Superhump period increased during the plateau phase.

Detected quasi-periodic oscillations at 104s and 188s.

Abstract

We present photometric observations of the dwarf nova 1RXS J053234.9+624755. We performed a detailed analysis of the superoutburst that occurred in August 2009. We found the superhump period to be P_sh=0.057122(14)days. Based on the O-C diagram we conclude that P_sh increased during the plateau at the rate of dP_sh/dt=(9.24 +- 1.4) * 10^-5. Both the O-C analysis and evolution of the superhumps light curve favour the model in which superhumps originate in a variable source located in the vicinity of the hot spot. In addition, the evolution of the light curve suggests that the superhump light source approaches the disc plane as the superoutburst declines. Detailed analysis of the superoutburst plateau phase enabled us to detect a signal which we interpret as apsidal motion of the accretion disc. We detected additional modulations during the final stage of the superoutburst characterized by periods of 104s and 188s which we tentatively interpret as quasi periodic oscillations. Estimations of A_0 and A_n are in agreement with the dependence discovered by Smak (2010) between the amplitude of superhumps and the orbital inclination.