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A comparative study of disc-planet interaction

Research output: Contribution to journalArticle

  • M. de Val-Borro
  • R. G. Edgar
  • P. Artymowicz
  • P. Ciecielag
  • P. Cresswell
  • G. D'Angelo
  • E. J. Delgado-Donate
  • G. Dirksen
  • S. Fromang
  • A. Gawryszczak
  • H. Klahr
  • W. Kley
  • W. Lyra
  • F. Masset
  • G. Mellema
  • R. P. Nelson
  • S.-J. Paardekooper
  • A. Peplinski
  • A. Pierens
  • T. Plewa
  • C. Schäfer
  • R. Speith

Related Edinburgh Organisations

Original languageEnglish
Pages (from-to)529-558
JournalMonthly Notices of the Royal Astronomical Society
Volume370
DOIs
Publication statusPublished - 1 Aug 2006

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 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.

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