2D radiation-hydrodynamical simulations find accretion outbursts unstable to Rossby-wave instability, forming vortices that suppress planetesimal formation until post-burst quiescence.
The effects of disc self-gravity and radiative cooling on the formation of gaps and spirals by young planets , volume =
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Nonlinear shock formation dominates angular momentum deposition from planet-induced density waves, cooling matches it for sub-thermal planets, and viscosity only matters at unrealistically high values.
Numerical experiments demonstrate that one migrating planet produces multiple long-lived dust rings and gaps in radiative discs through migration jumps, with cooling affecting jump count but not structure lifetime.
citing papers explorer
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Planet formation at the inner edge of the dead zone II. Outbursts, rings, vortices, and suppression of planetesimal formation
2D radiation-hydrodynamical simulations find accretion outbursts unstable to Rossby-wave instability, forming vortices that suppress planetesimal formation until post-burst quiescence.
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$\alpha\beta q_\mathrm{th}$-mapping of planet-induced density wave damping in protoplanetary discs
Nonlinear shock formation dominates angular momentum deposition from planet-induced density waves, cooling matches it for sub-thermal planets, and viscosity only matters at unrealistically high values.
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Formation of multiple dust rings and gaps in protoplanetary discs by a single migrating planet II: radiative discs and observational signatures
Numerical experiments demonstrate that one migrating planet produces multiple long-lived dust rings and gaps in radiative discs through migration jumps, with cooling affecting jump count but not structure lifetime.