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We herein develop a new simple model for giant planet formation, whichpredicts the final mass of a giant planet born in a given disk, by adding thedisk mass loss due to photoevaporation and a new type II migration formula toour previous model. The proposed model provides some interesting results.First, it gives universal evolution tracks in the diagram of planetary mass andorbital radius, which clarifies how giant planets migrate at growth in therunaway gas accretion stage. Giant planets with a few Jupiter masses or lesssuffer only a slight radial migration in the runaway gas accretion stage.Second, the final mass of giant planets is approximately given as a function ofonly three parameters: the initial disk mass at the starting time of runawaygas accretion onto the planet, the mass loss rate due to photoevaporation, andthe starting time. On the other hand, the final planet mass is almostindependent of the disk radius, viscosity, and initial orbital radius. Theobtained final planet mass is similar to or less than 10% of the initial diskmass. Third, the proposed model successfully explains properties in the massdistribution of giant exoplanets with the mass distribution of observedprotoplanetary disks for a reasonable range of the mass loss rate due tophotoevaporation.

Final Masses of Giant Planets III: Effect of Photoevaporation and a New Planetary Migration Model