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We present the results of 2-dimensional hydrodynamic simulations ofself-gravitating circumbinary discs around binaries whose parameters matchthose of the circumbinary planet-hosting systems Kepler-16, -34 and -35.Previous work has shown that non-self-gravitating discs in these systems forman eccentric precessing inner cavity due to tidal truncation by the binary, andplanets which form at large radii migrate until stalling at this cavity. Whilethis scenario appears to provide a natural explanation for the observed orbitallocations of the circumbinary planets, previous simulations have failed tomatch the observed planet orbital parameters. The aim of this work is toexamine the role of self-gravity in modifying circumbinary disc structure as afunction of disc mass, prior to considering the evolution of embeddedcircumbinary planets. In agreement with previous work, we find that for discmasses between 1--5 times the minimum mass solar nebula (MMSN), discself-gravity affects modest changes in the structure and evolution ofcircumbinary discs. Increasing the disc mass to 10 or 20 MMSN leads to twodramatic changes in disc structure. First, the scale of the inner cavityshrinks substantially, bringing its outer edge closer to the binary. Second, inaddition to the eccentric inner cavity, additional precessing eccentricring-like features develop in the outer regions of the discs. If planetformation starts early in the disc lifetime, these changes will have asignificant impact on the formation and evolution of planets and precursormaterial.

The Role of Disc Self-Gravity in Circumbinary Planet Systems: I. Disc Structure and Evolution