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Based on early Kepler data, Ostensen et al. (2010) found that KIC 9202990showed a 4 hr and a two-week photometric period. They suggested the 4 hr periodwas a signature of an orbital period; the longer period was possibly due toprecession of an accretion disk and KIC 9202990 was a cataclysmic variable withan accretion disk which is always in a bright state (a nova-like system). Usingthe full Kepler dataset on KIC 9202990 which covers 1421 d (Quarter 2--17), andincludes 1 min cadence data from the whole of Quarters 5 and 16, we find thatthe 4 hr period is stable and therefore a signature of the binary orbitalperiod. In contrast, the 10--12 d period is not stable and shows an amplitudebetween 20--50 percent. This longer period modulation is similar to thosenova-like systems which show `stunted' outbursts. We discuss the problems thata precessing disk model has in explaining the observed characteristics andindicate why we favour a stunted outburst model. Although such stunted eventsare considered to be related to the standard disk instability mechanism, theirorigin is not well understood. KIC 9202990 shows the lowest amplitude andshortest period of continuous stunted outburst systems, making it an idealtarget to better understand stunted outbursts and accretion instabilities ingeneral.

Continuous `stunted' outbursts detected from the Cataclysmic Variable KIC 9202990 using Kepler data