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Using a suite of numerical calculations, we consider the long-term evolutionof circumbinary debris from the Pluto-Charon giant impact. Initially, thesesolids have large eccentricity and pericenters near Charon's orbit. On timescales of 100-1000 yr, dynamical interactions with Pluto and Charon lead to theejection of most solids from the system. As the dynamics moves particles awayfrom the barycenter, collisional damping reduces the orbital eccentricity ofmany particles. These solids populate a circumbinary disk in the Pluto-Charonorbital plane; a large fraction of this material lies within a `satellite zone'that encompasses the orbits of Styx, Nix, Kerberos, and Hydra. Compared to thenarrow rings generated from the debris of a collision between a trans-Neptunianobject (TNO) and Charon, disks produced after the giant impact are much moreextended and may be a less promising option for producing small circumbinarysatellites.

A Pluto--Charon Concerto II. Formation of a Circumbinary Disk of Debris After the Giant Impact