  Based on early Kepler data, Ostensen et al. (2010) found that KIC 9202990
showed a 4 hr and a two-week photometric period. They suggested the 4 hr period
was a signature of an orbital period; the longer period was possibly due to
precession of an accretion disk and KIC 9202990 was a cataclysmic variable with
an accretion disk which is always in a bright state (a nova-like system). Using
the full Kepler dataset on KIC 9202990 which covers 1421 d (Quarter 2--17), and
includes 1 min cadence data from the whole of Quarters 5 and 16, we find that
the 4 hr period is stable and therefore a signature of the binary orbital
period. In contrast, the 10--12 d period is not stable and shows an amplitude
between 20--50 percent. This longer period modulation is similar to those
nova-like systems which show `stunted' outbursts. We discuss the problems that
a precessing disk model has in explaining the observed characteristics and
indicate why we favour a stunted outburst model. Although such stunted events
are considered to be related to the standard disk instability mechanism, their
origin is not well understood. KIC 9202990 shows the lowest amplitude and
shortest period of continuous stunted outburst systems, making it an ideal
target to better understand stunted outbursts and accretion instabilities in
general.
