An Investigation of 7 Non-eclipsing SU UMa Systems Using TESS Data

We present a study of seven non-eclipsing SU Ursae Majoris-type dwarf novae based on high-resolution photometric data obtained from the Transiting Exoplanet Survey Satellite (TESS). Our analysis focuses on the evolution of superhump periods during superoutbursts, which are key to understanding the tidal instability and accretion dynamics in these cataclysmic variable systems. By identifying and analyzing the characteristic stages A, B, and C of superhump evolution through the O-C method, we estimated the superhump periods for each system during the superoutburst. The Stage A superhump period, which corresponds to the initial growing phase of the superhumps, was used to estimate the mass ratio \( q = M_2/M_1 \) for each system using the method proposed by Kato and Osaki. Our results show that the mass ratios for these systems span a range from \(q \approx 0.07\) to \(q \approx 0.23\) , consistent with theoretical expectations for SU UMa-type systems.