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A Comparison of Numerical Simulations of Disk-Planet Interactions

Research output: Contribution to journalArticle

  • Miguel 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
  • F. Masset
  • G. Mellema
  • R. Nelson
  • S. J. Paardekooper
  • A. Peplinski
  • A. Pierens
  • T. Plewa
  • C. Schäfer
  • R. Speith

Related Edinburgh Organisations

Original languageEnglish
Pages (from-to)496
JournalBulletin of the American Astronomical Society
Volume39
Publication statusPublished - 1 Oct 2007

Abstract

We study the gravitational interaction between a protoplanetary disk and an embedded high-mass planet using several grid-based and smoothed particle hydrodynamics (SPH) schemes. Jupiter and Neptune mass planets are kept on a fixed circular orbit during several hundred orbital periods. We run tests for inviscid and viscous disks with Navier-Stokes viscosity of ν=10-5. We find good agreement between our codes. The averaged density profiles agree within 5%. SPH results have comparable shape of the gap and weaker planetary wakes than grid-based codes. Torque contributions from different parts in the disk and mass losses are monitored with high temporal resolution. High-density vortices are generated close to the coorbital region in the inviscid runs in agreement with the linear analysis. As the vortices move along the gap they introduce strong perturbations on the torque exerted on the planet. The smoothed total torques acting on the planet agree within a factor of 2 and the disk masses agree within 10% after 200 orbits.

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