How the planetary eccentricity influences the pebble isolation mass

ABSTRACT We investigate the pebble isolation mass (PIM) for a planet on fixed eccentric orbit in its protoplanetary disc by conducting set of two-dimensional (2D) hydrodynamical simulations, including dust turbulent diffusion. A range eccentricities up to e = 0.2 is adopted. Our simulations also cover ?-turbulent viscosities, and each pair {?, e} PIM estimated as minimum our such that solids with Stokes number ?0.05 do not flow across remain trapped around pressure bump outside gap. For ? < 10?3, we find planets reach well-defined PIM, which can be smaller than circular orbits when eccentricity remains disc’s aspect ratio. provide fitting formula how depends planet's eccentricity. However, > cannot fully stall pebbles and, thus, PIM. results suggest maximum reached rocky cores should exhibit dichotomy depending disc's viscosity. While being limited ${\cal O}(10\, M_\oplus)$ low-viscosity discs, this could much larger values discs high viscosity vicinity. further highlight filtering growing might effective previously thought, especially high-viscosity important implications observations.