Three-dimensional Disk-Planet Torques in a Locally Isothermal Disk

@article{DAngelo2010ThreedimensionalDT,
  title={Three-dimensional Disk-Planet Torques in a Locally Isothermal Disk},
  author={Gennaro D'Angelo and Stephen H. Lubow},
  journal={The Astrophysical Journal},
  year={2010},
  volume={724},
  pages={730-747}
}
We determine an expression for the Type I planet migration torque involving a locally isothermal disk, with moderate turbulent viscosity (5 × 10–4 α 0.05), based on three-dimensional nonlinear hydrodynamical simulations. The radial gradients (in a dimensionless logarithmic form) of density and temperature are assumed to be constant near the planet. We find that the torque is roughly equally sensitive to the surface density and temperature radial gradients. Both gradients contribute to inward… Expand
Planet-disk interaction in three dimensions: The importance of buoyancy waves
We carry out local three-dimensional (3D) hydrodynamic simulations of planet-disk interaction in stratified disks with varied thermodynamic properties. We find that whenever the Brunt-VaisalaExpand
Improved torque formula for low and intermediate mass planetary migration
The migration of planets on nearly circular, non-inclined orbits in protoplanetary discs is entirely described by the disc's torque. This torque is a complex function of the disc parameters, andExpand
Three-Dimensional Disc-Satellite Interaction: Torques, Migration, and Observational Signatures
The interaction of a satellite with a gaseous disk results in the excitation of spiral density waves which remove angular momentum from the orbit. In addition, if the orbit is not coplanar with theExpand
Planet-disc interaction in laminar and turbulent discs
In weakly ionized discs turbulence can be generated through the vertical shear instability (VSI). Embedded planets feel a stochastic component in the torques acting on them which can impact theirExpand
Planetary Torque in 3D Isentropic Disks
Planet migration is inherently a three-dimensional (3D) problem, because Earth-size planetary cores are deeply embedded in protoplanetary disks. Simulations of these 3D disks remain challenging dueExpand
Planets in turbulent Disks
Planets form in protoplanetary accretion disks around young protostars. These disks are driven by internal turbulence and the gas flow is in general not laminar but has stochastic components. ForExpand
Halting Migration: Numerical Calculations of Corotation Torques in the Weakly Nonlinear Regime
Planets in their formative years can migrate due to the influence of gravitational torques in the protoplanetary disk they inhabit. For low-mass planets in an isothermal disk, it is known that thereExpand
Low-mass planets in nearly inviscid disks: numerical treatment
Context. Embedded planets disturb the density structure of the ambient disk, and gravitational back-reaction possibly will induce a change in the planet’s orbital elements. Low-mass planets only haveExpand
Migration of protoplanets with surfaces through discs with steep temperature gradients
We perform three-dimensional self-gravitating radiative transfer simulations of protoplanet migration in circumstellar discs to explore the impact upon migration of the radial temperature profiles inExpand
On type-I migration near opacity transitions. A generalized Lindblad torque formula for planetary population synthesis
We give an expression for the Lindblad torque acting on a low-mass planet embedded in a protoplanetary disk that is valid even at locations where the surface density or temperature profile cannot beExpand
...
1
2
3
4
5
...

References

SHOWING 1-10 OF 41 REFERENCES
Planet migration in three-dimensional radiative discs
Context. The migration of growing protoplanets depends on the thermodynamics of the ambient disc. Standard modelling, using locally isothermal discs, indicate an inward (type-I) migration in the lowExpand
Type I Planet Migration in Nearly Laminar Disks
We describe two-dimensional hydrodynamic simulations of the migration of low-mass planets ( 30 M⊕) in nearly laminar disks (viscosity parameter α< 10 −3 ) over timescales of several thousand orbitExpand
Three-Dimensional Interaction between a Planet and an Isothermal Gaseous Disk. I. Corotation and Lindblad Torques and Planet Migration
Gravitational interaction between a planet and a three-dimensional isothermal gaseous disk is studied. In the present paper we mainly examine the torque on a planet and the resultant radial migrationExpand
Low-Mass Protoplanet Migration in T Tauri α-Disks
We present detailed estimates of type I-migration rates for low-mass protoplanets embedded in steady state T Tauri α-disks, based on Lindblad torque calculations ignoring feedback on the disk.Expand
The dependence of protoplanet migration rates on co-orbital torques
We investigate the migration rates of high-mass protoplanets embedded in accretion discs via two- and three-dimensional hydrodynamical simulations. The simulations follow the planet's radial motionExpand
Three-dimensional Simulations of a Planet Embedded in a Protoplanetary Disk
The dynamical influence of Jupiter-sized planets still embedded in protostellar disks is studied by means of numerical simulations. The three-dimensional structure of the disk is fully taken intoExpand
A comparative study of disc–planet interaction
We perform numerical simulations of a disc-planet system using various grid-based and smoothed particle hydrodynamics (SPH) codes. The tests are run for a simple setup where Jupiter and Neptune massExpand
Three-dimensional calculations of high- and low-mass planets embedded in protoplanetary discs
We analyse the non-linear, three-dimensional response of a gaseous, viscous protoplanetary disc to the presence of a planet of mass ranging from 1 Earth mass (1 M⊕) to 1 Jupiter mass (1 MJ) by usingExpand
Type I Migration in a Nonisothermal Protoplanetary Disk
We calculate rates of type I migration of protoplanets in a nonisothermal three-dimensional protoplanetary disk, building on planet-disk models developed in previous work. We find that including theExpand
ORBITAL MIGRATION AND MASS ACCRETION OF PROTOPLANETS IN THREE-DIMENSIONAL GLOBAL COMPUTATIONS WITH NESTED GRIDS
We investigate the evolution of protoplanets with different masses embedded in an accretion disk, via global fully three-dimensional hydrodynamical simulations. We consider a range of planetaryExpand
...
1
2
3
4
5
...