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How the planetary eccentricity influences the pebble isolation mass

Abstract : We investigate the pebble isolation mass (PIM) for a planet on a fixed eccentric orbit in its protoplanetary disc by conducting a set of two-dimensional (2D) hydrodynamical simulations, including dust turbulent diffusion. A range of planet eccentricities up to e = 0.2 is adopted. Our simulations also cover a range of α-turbulent viscosities, and for each pair {α, e} the PIM is estimated as the minimum planet mass in our simulations such that solids with a Stokes number ≳0.05 do not flow across the planet orbit and remain trapped around a pressure bump outside the planet gap. For α < 10-3, we find that eccentric planets reach a well-defined PIM, which can be smaller than for planets on circular orbits when the eccentricity remains smaller than the disc's aspect ratio. We provide a fitting formula for how the PIM depends on the planet's eccentricity. However, for α > 10-3, eccentric planets cannot fully stall the pebbles flow and, thus, do not reach a well-defined PIM. Our results suggest that the maximum mass reached by rocky cores should exhibit a dichotomy depending on the disc's turbulent viscosity. While being limited to ${\cal O}(10\, M_\oplus)$ in low-viscosity discs, this maximum mass could reach much larger values in discs with a high turbulent viscosity in the planet vicinity. Our results further highlight that pebble filtering by growing planets might not be as effective as previously thought, especially in high-viscosity discs, with important implications to protoplanetary discs observations.
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Submitted on : Monday, May 2, 2022 - 2:53:43 PM
Last modification on : Monday, July 4, 2022 - 9:34:54 AM

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Raúl O. Chametla, Frédéric S. Masset, Clément Baruteau, Bertram Bitsch. How the planetary eccentricity influences the pebble isolation mass. Monthly Notices of the Royal Astronomical Society, Oxford University Press (OUP): Policy P - Oxford Open Option A, 2022, 510 (3), pp.3867-3875. ⟨10.1093/mnras/stab3753⟩. ⟨insu-03656915⟩

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