The 2003 and 2005 superhumps in V1113 Cygni

TL;DR

This study presents CCD photometry of V1113 Cygni, confirming its classification as an SU UMa dwarf nova through superhump observations and revealing an exceptionally high rate of superhump period decrease during a superoutburst.

Contribution

First detailed CCD photometry of V1113 Cygni's superoutbursts, measuring superhump periods and their rapid decrease, confirming its SU UMa classification.

Findings

Superhump period of 0.07891 days detected.

Superhump period decreased at a rate of -4.5×10^{-4}.

V1113 Cygni confirmed as SU UMa dwarf nova.

Abstract

We report CCD photometry of the cataclysmic variable V1113 Cygni. During two campaigns, lasting from May to August 2003 and from March to June 2005, we recorded two superoutburst. In the obtained light curves we detected clear superhumps with a mean period 0.07891(3) days (113.63(4) min). That fact confirms that the star is a member of SU UMa class of dwarf novae. During the first observed superoutburst the superhump period was decreasing with an enormous rate of $\dot P = -4.5(8)\times 10^{-4}$ which is one of the highest values ever observed in SU UMa systems.