How to form compact & other longer-lived planet-induced vortices: VSI, planet migration, or re-triggers, but not feedback
arXiv:2304.01674 · doi:10.1093/mnras/stad2264
Abstract
Past computational studies of planet-induced vortices have shown that the dust asymmetries associated with these vortices can be long-lived enough that they should be much more common in mm/sub-mm observations of protoplanetary discs, even though they are quite rare. Observed asymmetries also have a range of azimuthal extents from compact to elongated even though computational studies have shown planet-induced vortices should be preferentially elongated. In this study, we use 2-D and 3-D hydrodynamic simulations to test whether those dust asymmetries should really be so long-lived or so elongated. With higher resolution (29 cells radially per scale height) than our previous work, we find that vortices can be more compact by developing compact cores when higher-mass planets cause them to re-form, or if they are seeded by tiny compact vortices from the vertical shear instability (VSI), but not through dust feedback in 3-D as was previously expected in general. Any case with a compact vortex or core(s) also has a longer lifetime. Even elongated vortices can have longer lifetimes with higher-mass planets or if the associated planet is allowed to migrate, the latter of which can cause the dust asymmetry to stop decaying as the planet migrates away from the vortex. These longer dust asymmetry lifetimes are even more inconsistent with observations, perhaps suggesting that discs still have an intermediate amount of effective viscosity.
24 pages, 21 figures; Published in MNRAS
References in corpus (39)
- Particle Stirring in Turbulent Gas Disks: Including Orbital Oscillations
- A Steeper than Linear Disk Mass-Stellar Mass Scaling Relation
- A comparative study of disc-planet interaction
- Vortex generation in protoplanetary disks with an embedded giant planet
- Convective Overstability in radially stratified accretion disks under thermal relaxation
- Type I planetary migration in a self-gravitating disk
- Treating gravity in thin disk simulations
- On the origin of horseshoes in transitional discs
- Effects of dust feedback on vortices in protoplanetary disks
- Convective overstability in accretion disks: 3D linear analysis and nonlinear saturation
- Anisotropic Infall and Substructure formation in Embedded Disks
- Dust-trapping vortices and a potentially planet-triggered spiral wake in the pre-transitional disk of V1247 Orionis
- Vortices and spirals in the HD135344B transition disk
- Long Term Evolution of Planet-Induced Vortices in Protoplanetary Disks
- Dust traps in the protoplanetary disc MWC 758: two vortices produced by two giant planets?
- Slowly-growing gap-opening planets trigger weaker vortices
- Thermodynamics of Giant Planet Formation: Shocking Hot Surfaces on Circumplanetary Disks
- Signatures of an eccentric disc cavity: Dust and gas in IRS 48
- High Resolution Parameter Study of the Vertical Shear Instability
- Influence of planetary gas accretion on the shape and depth of gaps in protoplanetary discs
- Steady State by Recycling prevents Premature Collapse of Protoplanetary Atmospheres
- Type III migration in a low viscosity disc
- Dynamical Evidence of a Spiral Arm--Driving Planet in the MWC 758 Protoplanetary Disk
- Migration of Jupiter mass planets in low viscosity discs
- Vortex-like kinematic signal, spirals, and beam smearing effect in the HD 142527 disk
- Stratified and vertically-shearing streaming instabilities in protoplanetary disks
- Gap formation and stability in non-isothermal protoplanetary discs
- Which planets trigger longer-lived vortices: low-mass or high-mass?
- Wavelike nature of the vertical shear instability in global protoplanetary disks
- Dust traps as planetary birthsites: basics and vortex formation
- Planet-disc interaction in laminar and turbulent discs
- Emergence of vortices at the edges of planet-driven gaps in protoplanetary discs
- The impact of dust evolution on the dead zone outer edge in magnetized protoplanetary disks
- Extreme Pebble Accretion in Ringed Protoplanetary Discs
- Gas accretion onto Jupiter mass planets in discs with laminar accretion flows
- Hydrodynamic turbulence in disks with embedded planets
- Dust rings as a footprint of planet formation in a protoplanetary disk
- Simultaneous gas accretion onto a pair of giant planets: Impact on their final mass and on the protoplanetary disk structure
- Multiple Rings and Asymmetric Structures in the Disk of SR 21