学术文献库

We study the effect of a migrating planet ($10<M_p<20$ Earth mass) on the dynamics of pebbles in a radiative disk using 2D two-fluid simulations carried out with the RoSSBi code. The combined action of the waves induced by the migrating planet and drag back-reaction on the gas produces a complex evolution of the flux of pebbles. The waves excite zonal flows which act as dust traps, and accumulate pebbles. Owing to drag back-reaction, a Kelvin-Helmholtz instability develops, generating turbulent dust rings containing several Earth masses of solids, where planetesimal formation is likely. The more massive the planet, the faster the dust rings develop. In competition with planet migration, this process triggers several dust rings, with a radial separation scaling as $1/M_p$. We discover a transition around $13$ Earth masses. Below that, pebbles are stopped at the inner side of the planet's orbit, but pebble accretion on the planet is sustained. Above that, drag back-reaction in the dust ring region flattens the pressure profile while the planet migrates, which limits further growth by pebble accretion. This new {\it pebble isolation mass} is about a factor of 2 lower than often reported in the literature. This reduces the overall formation timescale of Super-Earth planets, while favoring their survival after the disk's dissipation because further accretion is stifled. Finally, our results support an hybrid model for the formation of Jupiter via both pebbles and planetesimals accretion.