We present detailed computations of the limit cycle model for dwarf nova outbursts with application to SS Cygni, the best studied dwarf nova. We examine how secular changes in the input parameters of the model affect the properties associated with the outbursts. For input parameters which reproduce the observed outburst recurrence times and outburst durations for SS Cyg, our time-dependent, accretion disk instability code generates light curves in which one or more short outbursts tend to be sandwiched between two long outbursts. We find that the relative frequency of long versus short outbursts can be influenced by changes in the accretion disk viscosity and mass transfer rate