Magnetospheric accretion is an important process for a wide range of astrophysical systems, and may play a role in the formation of gas giant planets. Extending the formalism describing stellar magnetospheric accretion into the planetary regime, we d
emonstrate that magnetospheric processes may govern accretion onto young gas giants in the isolation phase of their development. Planets in the isolation phase have cleared out large gaps in their surrounding circumstellar disks, and settled into a quasi-static equilibrium with radii only modestly larger than their final sizes (i.e., $ r sim 1.4 r_{rm final}$). Magnetospheric accretion is less likely to play a role in a young gas giants main accretion phase, when the planets envelope is predicted to be much larger than the planets Alfven radius. For a fiducial 1 M$_J$ gas giant planet with a remnant isolation phase accretion rate of $dot{M}_{odot} =$ 10$^{-10} M_{odot}{rm yr}^{-1}=10^{-7}M_{J}{rm yr}^{-1}$, the disk accretion will be truncated at $sim 2.7r_J$ (with $r_J$ is Jupiters radius) and drive the planet to rotate with a period of $sim$7 hours. Thermal emission from planetary magnetospheric accretion will be difficult to observe; the most promising observational signatures may be non-thermal, such as gyrosynchrotron radiation that is clearly modulated at a period much shorter than the rotation period of the host star.
