2013MNRAS.431.1903W

We investigate the kinematic evolution of planetesimals in self-gravitating discs, combining smoothed particle hydrodynamical (SPH) simulations of the disc gas with a gravitationally coupled population of test particle planetesimals. We find that at radii of tens of au (which is where we expect planetesimals to be possibly formed in such discs), the planetesimals' eccentricities are rapidly pumped to values >0.1 within the time-scales for which the disc is in the self-gravitating regime. The high resulting velocity dispersion and the lack of planetesimal concentration in the spiral arms means that the collision time-scale is very long and that the effect of those collisions that do occur is destructive rather than leading to further planetesimal growth. We also use the SPH simulations to calibrate Monte Carlo dynamical experiments: these can be used to evolve the system over long time-scales and can be compared with analytical solutions of the diffusion equation in particle angular momentum space. We find that if planetesimals are only formed in a belt at large radius, then there is significant scattering of objects to small radii; nevertheless, the majority of planetesimals remain at large radii. If planetesimals indeed form at early evolutionary stages, when the disc is strongly self-gravitating, then the results of this study constrain their spatial and kinematic distribution at the end of the self-gravitating phase.