  We use simulated planetary systems to model the planet multiplicity of Kepler
stars. Previous studies have underproduced single planet systems and invoked
the so called Kepler dichotomy, where the planet forming ability of a Kepler
star is dichotomous, producing either few or many transiting planets. In this
paper we show that the Kepler dichotomy is only required when the inner part of
planetary disks are just assumed to be flared. When the inner part of planetary
disks are flat, we reproduce the observed planet multiplicity of Kepler stars
without the need to invoke a dichotomy. We find that independent of the disk
model assumed, the mean number of planets per star is approximately 2 for
orbital periods between 3 and 200 days, and for planetary radii between 1 and 5
Earth radii. This contrasts with the Solar System where no planets occupy the
same parameter space.
