A comparative study of disc–planet interaction

By Miguel de Val-Borro, R. Edgar, P. Artymowicz, P. Ciecielag, P. Cresswell, G. D’Angelo, E. Delgado-Donate, G. Dirksen, Sébastien Fromang, A. Gawryszczak and 13 more. 2006

308 citations recorded by the source corpus.

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 mass planets on a circular orbit open a gap in a protoplanetary disc during a few hundred orbital periods. We compare the surface density contours, potential vorticity and smoothed radial profiles at several times. The disc mass and gravitational torque time evolution are analysed with high temporal resolution. There is overall consistency between the codes. The density profiles agree within about 5 per cent for the Eulerian simulations. The SPH results predict the correct shape of the gap although have less resolution in the low-density regions and weaker planetary wakes. The disc masses after 200 orbital periods agree within 10 per cent. The spread is larger in the tidal torques acting on the planet which agree within a factor of 2 at the end of the simulation. In the Neptune case, the dispersion in the torques is greater than for Jupiter, possibly owing to the contribution from the not completely cleared region close to the planet.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/25d8827b24f543530fe56a607addfb7d8354cab5

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Citations in the corpus

On planet formation in HL Tau (2015, background): “First, prominent spiral waves induced by the planet are seen in all theoretical simulations of planets carving gaps in gas discs whenever the planet is massive enough to open a gap (e.g.de Val-Borro et al. 2006).”
On the Corotation Torque in a Radiatively Inefficient Disk (2007, methodology): “Despite this precaution, wave killing zones next to the boundaries were implemented to minimize unphysical wave reflections (de Val-Borro et al. 2006).”
Phantom: A Smoothed Particle Hydrodynamics and Magnetohydrodynamics Code for Astrophysics (2017, methodology): “Despite the different assumptions, the results in Figure 22 are strikingly similar to those obtained with most of the grid-based codes in de Val-Borro et al. (2006).”
The subcritical baroclinic instability in local accretion disc models (2009, background): “…the literature to justify the existence of these vortices such as Rossby wave instabilities (Lovelace et al. 1999), planetary gap instabilities (de Val-Borro et al. 2006, 2007), 3D circulation models (Barranco & Marcus 2005), MHD turbulence (Fromang & Nelson 2005) and the global baroclinic…”
Planet formation bursts at the borders of the dead zone in 2D numerical simulations of circumstellar disks (2009, methodology): “Both use the buffer zone described in de Val-Borro et al. (2006) to damp waves before they reach the boundary.”
A torque formula for non-isothermal type I planetary migration – I. Unsaturated horseshoe drag (2009, background): “This instability is usually discussed in the context of giant, gap opening planets (Li et al. 2005; de Val-Borro et al. 2007), for which it was observed in most numerical codes for inviscid discs (de Val-Borro et al. 2006).”
Ring shaped dust accumulation in transition disks (2012, unknown): “The gap is replenished easily because of the high viscosity of the disk as already predicted by different authors (e.g de Val-Borro et al. 2006; Crida et al. 2006).”
Radial Migration of Gap-opening Planets in Protoplanetary Disks. I. The Case of a Single Planet (2018, methodology): “To avoid an artificial wave reflection, the damping is used in the so-called wave-killing zone near the boundary layers (cf., de Val-Borro et al. 2006).”
Planet-Disk Interaction and Orbital Evolution (2012, background): “Because there are a number of codes on the market, a detailed code comparison project was conducted a few years ago to verify the convergence of the results (de Val-Borro et al., 2006).”
HOW EMPTY ARE DISK GAPS OPENED BY GIANT PLANETS (2013, background): “These streamers, which de Val-Borro et al. (2006) called “filaments”, are prominent in the high-q snapshots in a Averaged over time and over a partial annulus centered on theplanet, as defined in§2.3.4 and delineated in Figures 3 and 4.”
TRANSITIONAL AND PRE-TRANSITIONAL DISKS: GAP OPENING BY MULTIPLE PLANETS? (2010, methodology): “8) In performing these tests with the indirect terms we found it necessary to adopt the wave-damping boundary condition described in De Val-Borro et al. (2006) in order for the disk to remain well behaved at the outside edge.”
Standing on the shoulders of giants : Trojan Earths and vortex trapping in low mass self-gravitating protoplanetary disks of gas and solids (2008, methodology): “To avoid giving the gas and the particles too much impulse when the planet is introduced in the unperturbed disk, we ramp its mass up from 0 to its final mass in five orbits, in the way described in de Val-Borro et al. (2006).”