  The wide, deep cavities of transition disks are often believed to have been
hollowed out by nascent planetary systems. PDS 70, a ${\sim}5$ Myr old
transition disk system in which a multi-Jupiter-mass planet candidate at 22 au
coexists with a ${\sim}30$ au gas and ${\sim}60$ au dust-continuum gap,
provides a valuable case study for this hypothesis. Using the PEnGUIn
hydrodynamics code, we simulate the orbital evolution and accretion of PDS 70b
in its natal disk over the lifetime of the system. When the accreting planet
reaches about 2.5 Jupiter masses, it spontaneously grows in eccentricity and
consumes material from a wide swathe of the PDS 70 disk; radiative transfer
post-processing with DALI shows that this accurately reproduces the observed
gap profile. Our results demonstrate that super-Jupiter planets can
single-handedly carve out transition disk cavities, and indicate that the high
eccentricities measured for such giants may be a natural consequence of
disk-planet interaction.
