2D radiation-hydrodynamical simulations find accretion outbursts unstable to Rossby-wave instability, forming vortices that suppress planetesimal formation until post-burst quiescence.
On the width and shape of gaps in protoplanetary disks
3 Pith papers cite this work. Polarity classification is still indexing.
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Pith papers citing it
abstract
Although it is well known that a massive planet opens a gap in a proto-planetary gaseous disk, there is no analytic description of the surface density profile in and near the gap. The simplest approach, which is based upon the balance between the torques due to the viscosity and the gravity of the planet and assumes local damping, leads to gaps with overestimated width, especially at low viscosity. Here, we take into account the fraction of the gravity torque that is evacuated by pressure supported waves. With a novel approach, which consists of following the fluid elements along their trajectories, we show that the flux of angular momentum carried by the waves corresponds to a pressure torque. The equilibrium profile of the disk is then set by the balance between gravity, viscous and pressure torques. We check that this balance is satisfied in numerical simulations, with a planet on a fixed circular orbit. We then use a reference numerical simulation to get an ansatz for the pressure torque, that yields gap profiles for any value of the disk viscosity, pressure scale height and planet to primary mass ratio. Those are in good agreement with profiles obtained in numerical simulations over a wide range of parameters. Finally, we provide a gap opening criterion that simultaneously involves the planet mass, the disk viscosity and the aspect ratio.
years
2026 3verdicts
UNVERDICTED 3representative citing papers
Semi-analytical models show AGN disks produce repeated BBH mergers with a high-mass tail beyond the pair-instability gap, more efficiently at low viscosity, with spin and mass-ratio signatures that can match events like GW190521.
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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AGN-driven BBH mergers: Black hole populations and hierarchical growth across the AGN parameter space
Semi-analytical models show AGN disks produce repeated BBH mergers with a high-mass tail beyond the pair-instability gap, more efficiently at low viscosity, with spin and mass-ratio signatures that can match events like GW190521.
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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.