CC Sculptoris: Eclipsing SU UMa-Type Intermediate Polar

TL;DR

This study presents detailed observations of the 2014 superoutburst of CC Scl, an eclipsing SU UMa-type intermediate polar, revealing superhump periods, system parameters, and the applicability of the thermal-tidal instability model.

Contribution

First detailed superoutburst analysis of CC Scl, confirming its classification and demonstrating the disk behavior aligns with the thermal-tidal instability model despite magnetic truncation.

Findings

Detected superhumps with a mean period of 0.05998 days.

Measured an orbital period of 0.058567 days.

Estimated a mass ratio of 0.072.

Abstract

We observed the 2014 superoutburst of the SU UMa-type intermediate polar CC Scl. We detected superhumps with a mean period of 0.05998(2) d during the superoutburst plateau and during three nights after the fading. During the post-superoutburst stage after three nights, a stable superhump period of 0.059523(6) d was detected. We found that this object is an eclipsing system with an orbital period of 0.058567233(8) d. By assuming that the disk radius in the post-superoutburst phase is similar to those in other SU UMa-type dwarf novae, we obtained a mass ratio of q=0.072(3) from the dynamical precession rate of the accretion disk. The eclipse profile during outbursts can be modeled by an inclination of 80.6+/-0.5 deg. The 2014 superoutburst was preceded by a precursor outburst and the overall appearance of the outburst was similar to superoutbursts in ordinary SU UMa-type dwarf novae. We showed that the standard thermal-tidal instability model can explain the outburst behavior in this system and suggest that inner truncation of the disk by magnetism of the white dwarf does not strongly affect the behavior in the outer part of the disk.