  We describe the evolution of low mass planets in a dispersing protoplanetary
disk around a Solar mass star. The disk model is based on the results of Yu,
Hansen & Hasegawa (2023), which describes a region of the inner disk where the
direction of the migration torque is outwards due to the diffusion of the
stellar magnetic field into the disk and the resultant gradual increase in
surface density outwards. We demonstrate that the magnetospheric rebound phase
in such a disk leads to diverging orbits for double and triple planet systems,
and the disruption of a high fraction of the initial resonant chains.
  We present simulations of three planet systems with masses based on the
observed triple planet systems observed by the Kepler satellite within the
context of this model. The final distribution of nearest neighbour period
ratios provides an excellent fit to the observations, provided that the initial
resonant configurations are compact. The occurrence rate of planets as a
function of orbital period also provides a good match to the observations, for
final orbital periods P<20 days.
  These results suggest that the period and period ratio distributions of low
mass planets are primarily set in place during the disk dispersal epoch, and
may not require significant dynamical evolution thereafter.
