Abstract

In recent years numerous circumbinary planets have been discovered- just exterior to the dynamical stability limit. The formation processes of such planets remains an unsolved problem. Forming planets close to the stability limit has proven difficult to achieve due to large relative velocities that result from interactions with the central binary stars. Recent hydrodynamical simulations have shown that tidal torques from the central binary act to form eccentric cavities within the circumbinary discs typically extending just past the stability limit with the sizes and properties of such cavities depending on both the binary and local disc properties. One advantage of such eccentric cavities is that they act as barriers to planet migration due to positive pressure gradients. In this presentation I will present results on the evolution of circumbinary discs containing dust species of varying size and abundance. The effects of the dust not only on the disc but also on the implications for planet formation will be discussed. I will then present the results of Nbody simulations around circumbinary stars such as Kepler-16 and Kepler-34. These simulations include the formation of planets through either pebble or planetesimal accretion within a 1D viscously evolving circumbinary disc. The circumbinary disc includes 2D prescriptions for an eccentric precessing cavity based on results from hydrodynamical simulations. We also include prescriptions for photoevaporation planet migration and gas accretion. The results of such simulations show that the pebble accretion scenarios are able to produce planetary systems orbiting close to the central binary stars. In particular, simulations are able to produce planets akin to Kepler-16b and Kepler-34b. I will finally discuss formation scenarios for BEBOP -1 including planetesimal and embryo formation, within a wide parameter space. The results of these simulations are able to give hints on the physical properties within circumbinary and protoplanetary discs.