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We present models of giant planet migration in evolving protoplanetary disks.Our disks evolve subject to viscous transport of angular momentum andphotoevaporation, while planets undergo Type II migration. We use a Monte Carloapproach, running large numbers of models with a range in initial conditions.We find that relatively simple models can reproduce both the observed radialdistribution of extra-solar giant planets, and the lifetimes and accretionhistories of protoplanetary disks. The use of state-of-the-art photoevaporationmodels results in a degree of coupling between planet formation and diskclearing, which has not been found previously. Some accretion across planetaryorbits is necessary if planets are to survive at radii <~1.5AU, and if planetsof Jupiter mass or greater are to survive in our models they must be able toform at late times, when the disk surface density in the formation region islow. Our model forms two different types of "transitional" disks, embeddedplanets and clearing disks, which show markedly different properties. We findthat the observable properties of these systems are broadly consistent withcurrent observations, and highlight useful observational diagnostics. Wepredict that young transition disks are more likely to contain embedded giantplanets, while older transition disks are more likely to be undergoing diskclearing.

Giant planet migration, disk evolution, and the origin of transitional disks