  We numerically study the precessing disk model for superhump in the SU~UMa
subclass of cataclysmic variables, using a two dimensional SPH code
specifically designed for thin disk problems.
  Two disk simulations for a binary with mass ratio $q=\frac{3}{17}$ (similar
to OY~Car) are performed, in order to investigate the Lubow (1991 a,b) tidal
resonance instability mechanism. In the first calculation, a disk evolves under
steady mass transfer from $L_1$. In the second simulation, mass is added in
Keplerian orbit to the inner disk.
  The two disks follow similar evolutionary paths. However the $L_1$
stream-disk interaction is found to slow the disk's radial expansion and to
circularise gas orbits.
  The initial eccentricity growth in our simulations is exponential at a rate
slightly less than predicted by Lubow (1991a). We do not observe a clearing of
material from the resonance region via the disk's tidal response to the $m=2$
component of the binary potential as was described in Lubow (1992). Instead the
$m=2$ response weakens as the disk eccentricty increases.
  Both disks reach an eccentric equilibrium state, in which they undergo
prograde precession. The rate of viscous energy dissipation in the disks has a
periodic excess with a period matching the disk's rotation. The source is
identified as a large region in the outer disk, and the mechanism by which it
is produced is identified. The time taken for the periodic excess to develop is
consistent with the first appearance of superhumps in a superoutburst.
