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Title:
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.; Rice, K.; Schäfer, C.; Speith, R.
Affiliation:
AA(Stockholm University, AlbaNova University Centre, SE-106 91, Stockholm, Sweden), AB(Stockholm University, AlbaNova University Centre, SE-106 91, Stockholm, Sweden; Department of Physics and Astronomy, University of Rochester, NY 14627, USA), AC(Stockholm University, AlbaNova University Centre, SE-106 91, Stockholm, Sweden; University of Toronto at Scarborough, 1265 Military Trail, Toronto, Ontario M1C 1A4, Canada), AD(University Observatory Munich, Scheinerstr. 1, D-81679 Munich, Germany; Nicolaus Copernicus Astronomical Centre, Bartycka 18, Warsaw, PL-00-716, Poland), AE(Astronomy Unit, Queen Mary, University of London, Mile End Road, London E1 4NS), AF(School of Physics, University of Exeter, Stocker Road, Exeter EX4 4QL), AG(Stockholm University, AlbaNova University Centre, SE-106 91, Stockholm, Sweden), AH(Institute of Astronomy and Astrophysics Tübingen, Auf der Morgenstelle 10, D-72076 Tübingen, Germany), AI(Astronomy Unit, Queen Mary, University of London, Mile End Road, London E1 4NS; DAMTP, University of Cambridge, Centre for Mathematical Sciences, Wilberforce Road, Cambridge CB3 0WA), AJ(Nicolaus Copernicus Astronomical Centre, Bartycka 18, Warsaw, PL-00-716, Poland), AK(Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany), AL(Institute of Astronomy and Astrophysics Tübingen, Auf der Morgenstelle 10, D-72076 Tübingen, Germany), AM(Department of Astronomy & Space Physics, Uppsala Astronomical Observatory, Box 515, 751 20, Sweden), AN(AIM, UMR 7158 CEA/CNRS/Univ. Paris VII, Service d'Astrophysique, Saclay, 91191 Gif-sur-Yvette Cedex, France; IA-UNAM, Ciudad Universitaria, Apartado Postal 70-264, Mexico DF 04510, Mexico), AO(Leiden Observatory, PO Box 9513, NL-2300 RA Leiden, the Netherlands), AP(Astronomy Unit, Queen Mary, University of London, Mile End Road, London E1 4NS), AQ(Leiden Observatory, PO Box 9513, NL-2300 RA Leiden, the Netherlands), AR(Stockholm University, AlbaNova University Centre, SE-106 91, Stockholm, Sweden), AS(Astronomy Unit, Queen Mary, University of London, Mile End Road, London E1 4NS; Luth, Observatoire de Paris-Meudon, 92 195 Meudon Cedex, France), AT(ASC FLASH Center, University of Chicago, 5640 South Ellis, Chicago, IL 60637, USA), AU(Scottish Universities Physics Alliance, Institute for Astronomy, University of Edinburgh, Blackford Hill, Edinburgh EH9 3HJ), AV(Institute of Astronomy and Astrophysics Tübingen, Auf der Morgenstelle 10, D-72076 Tübingen, Germany), AW(Institute of Astronomy and Astrophysics Tübingen, Auf der Morgenstelle 10, D-72076 Tübingen, Germany)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 370, Issue 2, pp. 529-558. (MNRAS Homepage)
Publication Date:
08/2006
Origin:
MNRAS
Astronomy Keywords:
accretion, accretion discs: hydrodynamics: planets and satellites: general, accretion discs, hydrodynamics, planets and satellites: general
DOI:
10.1111/j.1365-2966.2006.10488.x
Bibliographic Code:
2006MNRAS.370..529D

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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