  Here a physical model for terminating giant planet formation is outlined and
compared to other methods of late-stage giant planet formation. As has been
pointed out before, gas accreting into a gap and onto the planet will encounter
the planetary dynamo-generated magnetic field. The planetary magnetic field
produces an effective cross section through which gas is accreted. Gas outside
this cross section is recycled into the protoplanetary disk, hence only a
fraction of mass that is accreted into the gap remains bound to the planet.
This cross section inversely scales with the planetary mass, which naturally
leads to stalled planetary growth late in the formation process. We show that
this method naturally leads to Jupiter-mass planets and does not invoke any
artificial truncation of gas accretion, as has been done in some previous
population synthesis models. The mass accretion rate depends on the radius of
the growing planet after the gap has opened, and we show that so-called
hot-start planets tend to become more massive than cold-start planets. When
this result is combined with population synthesis models, it might show
observable signatures of cold-start versus hot-start planets in the exoplanet
population.
