3:30 PM - 3:45 PM
[PPS07-13] Planetesimal rings formed by the "No-drift" mechanism
Keywords:planetesimals, protoplanetary disks, planet formation
Forming planetesimals from pebbles is a major challenge in our current understanding of planet formation. In gas disks, pebbles drift inward near the disk midplane due to gas drag and they may enter a dead zone. In this context, we reported that a pebble-gas backreaction to the radial drift of pebbles could lead to a runaway accumulation of pebbles, the so-called no-drift mechanism (Hyodo, Ida, Guillot 2021, A&A Letters).
Here, we additionally performed 1D diffusion-advection simulations of drifting pebbles in the outer region of a dead zone by including the backreaction to the radial drift of pebbles and including planetesimal formation via the streaming instability.
When the no-drift mechanism is realized, we find that planetesimals initially form within a narrow ring whose width expands as accumulating pebbles radially diffuse over time. The system finally reaches a steady-state, where the width of the planetesimal belt no longer changes. We show a non-negligible total mass of planetesimals (more than one Earth mass) is formed by the no-drift mechanism (Hyodo, Ida, Guillot 2021, A&A).
Here, we additionally performed 1D diffusion-advection simulations of drifting pebbles in the outer region of a dead zone by including the backreaction to the radial drift of pebbles and including planetesimal formation via the streaming instability.
When the no-drift mechanism is realized, we find that planetesimals initially form within a narrow ring whose width expands as accumulating pebbles radially diffuse over time. The system finally reaches a steady-state, where the width of the planetesimal belt no longer changes. We show a non-negligible total mass of planetesimals (more than one Earth mass) is formed by the no-drift mechanism (Hyodo, Ida, Guillot 2021, A&A).