The outburst of V713 Cephei in August 2009

TL;DR

This paper reports precise orbital period measurements of V713 Cephei during its 2009 outburst, noting the absence of superhumps and analyzing eclipse depth variations related to system excitation.

Contribution

It provides an improved orbital period and detailed eclipse analysis of V713 Cephei during outburst and quiescence, highlighting the system's high inclination and eclipse characteristics.

Findings

Orbital period refined to 0.085418432(4) days.

Eclipse depth decreases linearly with system excitation.

No superhumps observed during outburst.

Abstract

During the outburst of V713 Cephei in August 2009 the times of 8 eclipses were measured and these, together with 5 eclipse timings obtained during quiescence in August 2007, provide an improved orbital period of 0.085418432(4)d. No superhumps were observed in the light curve indicating this was a normal UG-type dwarf nova outburst. We found the eclipse depth decreased linearly with rising system excitation level, falling from ~3 magnitudes in quiescence to ~2 magnitudes during outburst. The depth and totality of eclipses in quiescence suggests a high orbital inclination. We saw no variation in the FWHM of eclipses between quiescence and outburst despite a significant change in shape of the eclipse profile.