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A comparative study of disc-planet interaction

Authors
  • de Val-Borro, M.
  • Edgar, R. G.
  • Artymowicz, P.
  • Ciecielag, P.
  • Cresswell, P.
  • D'Angelo, G.
  • Delgado-Donate, E. J.
  • Dirksen, G.
  • Fromang, S.
  • Gawryszczak, A.
  • Klahr, H.
  • Kley, W.
  • Lyra, W.
  • Masset, F.
  • Mellema, G.
  • Nelson, R. P.
  • Paardekooper, S. -J.
  • Peplinski, A.
  • Pierens, A.
  • Plewa, T.
  • And 3 more
Type
Published Article
Publication Date
Jun 01, 2006
Submission Date
May 09, 2006
Identifiers
DOI: 10.1111/j.1365-2966.2006.10488.x
Source
arXiv
License
Unknown
External links

Abstract

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 analyzed with high temporal resolution. There is overall consistency between the codes. The density profiles agree within about 5% for the Eulerian simulations while 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%. The spread is larger in the tidal torques acting on the planet which agree within a factor 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.

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