A comparative study of disc-planet interaction
Miguel de Val-Borro
(1)
,
R. G. Edgar
(1)
,
P. Artymowicz
(1)
,
P. Ciecielag
(2)
,
P. Cresswell
(3)
,
G. d'Angelo
(4)
,
E. J. Delgado-Donate
(1)
,
G. Dirksen
(5)
,
Sébastien Fromang
(3)
,
A. Gawryszczak
(6)
,
Hubert Klahr
(7)
,
Willy Kley
(5)
,
W. Lyra
(8)
,
Frédéric Masset
(9, 10)
,
Garrelt Mellema
(11)
,
Richard P. Nelson
(3)
,
Sijme-Jan Paardekooper
(11)
,
A. Peplinski
(1)
,
Arnaud Pierens
(3, 12)
,
T. Plewa
(13)
,
K. Rice
(14)
,
C. Schäfer
(5)
,
R. Speith
(5)
1
Stockholm University
2 University Observatory Munich, Ludwig-Maximillians University Munich
3 School of Mathematical Sciences, Queen Mary Unversity of London
4 University of Exeter
5 Eberhard Karls Universität Tübingen = Eberhard Karls University of Tuebingen
6 CAMK - Centrum Astronomiczne im. M. Kopernika, Warszawa
7 MPIA - Max-Planck-Institut für Astronomie
8 Department of Astronomy and Space Physics, Uppsala Astronomical Observatory
9 CEA - Commissariat à l'énergie atomique et aux énergies alternatives
10 Instituto de Astronomia, Universidad Nacional Autonomica de Mexico
11 Leiden Observatory
12 LUTH (UMR_8102) - Laboratoire Univers et Théories
13 University of Chicago, ASC FLASH Center
14 Edin. - University of Edinburgh
2 University Observatory Munich, Ludwig-Maximillians University Munich
3 School of Mathematical Sciences, Queen Mary Unversity of London
4 University of Exeter
5 Eberhard Karls Universität Tübingen = Eberhard Karls University of Tuebingen
6 CAMK - Centrum Astronomiczne im. M. Kopernika, Warszawa
7 MPIA - Max-Planck-Institut für Astronomie
8 Department of Astronomy and Space Physics, Uppsala Astronomical Observatory
9 CEA - Commissariat à l'énergie atomique et aux énergies alternatives
10 Instituto de Astronomia, Universidad Nacional Autonomica de Mexico
11 Leiden Observatory
12 LUTH (UMR_8102) - Laboratoire Univers et Théories
13 University of Chicago, ASC FLASH Center
14 Edin. - University of Edinburgh
Résumé
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.