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Two longstanding problems in planet formation include (1) understanding howplanets survive migration, and (2) articulating the process by whichprotoplanetary disks disperse---and in particular how they accrete onto theircentral stars. We can go a long way toward solving both problems if the diskgas surrounding planets has no intrinsic diffusivity ("viscosity"). Ininviscid, laminar disks, a planet readily repels gas away from its orbit. Onshort timescales, zero viscosity gas accumulates inside a planet's orbit toslow Type I migration by orders of magnitude. On longer timescales, multiplesuper-Earths (distributed between, say, $\sim$0.1--10 AU) can torque inviscidgas out of interplanetary space, either inward to feed their stars, or outwardto be blown away in a wind. We explore this picture with 2D hydrodynamicssimulations of Earths and super-Earths embedded in inviscid disks, confirmingtheir slow/stalled migration even under gas-rich conditions, and showing thatdisk transport rates range up to $\sim$$10^{-7} M_\odot~{\rm yr^{-1}}$ andscale as $\dot{M} \propto \Sigma M_{\rm p}^{3/2}$, where $\Sigma$ is the disksurface density and $M_{\rm p}$ is the planet mass. Gas initially sandwichedbetween two planets is torqued past both into the inner and outer disks. Insum, sufficiently compact systems of super-Earths can clear their natal diskgas, in a dispersal history that may be complicated and non-steady, but whichconceivably leads over Myr timescales to large gas depletions similar to thosecharacterizing transition disks.

Save the Planet, Feed the Star: How Super-Earths Survive Migration and Drive Disk Accretion