Open AccessOn the migration of a system of protoplanets
Author(s) -
Kley W.
Publication year - 2000
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-8711.2000.03495.x
Subject(s) - physics , planet , protoplanet , jupiter mass , exoplanet , jupiter (rocket family) , accretion (finance) , planetary mass , planetary system , astrophysics , radius , planetary migration , gravitation , astronomy , gas giant , protoplanetary disk , computer security , space shuttle , computer science
The evolution of a system consisting of a protoplanetary disc with two embedded Jupiter‐sized planets is studied numerically. The disc is assumed to be flat and non‐self‐gravitating; this is modelled by the planar (two‐dimensional) Navier–Stokes equations. The mutual gravitational interaction of the planets and the star, and the gravitational torques of the disc acting on the planets and the central star are included. The planets have an initial mass of one Jupiter mass M Jup each, and the radial distances from the star are one and two semimajor axes of Jupiter, respectively. During the evolution a joint wide annular gap is created by the planets. Both planets increase their mass owing to accretion of gas from the disc: after about 2500 orbital periods of the inner planet it has reached a mass of 2.3 M Jup , while the outer planet has reached a mass of 3.2 M Jup . The net gravitational torques exerted by the disc on the planets result in an inward migration of the outer planet on time‐scales comparable to the viscous evolution time of the disc. The semimajor axis of the inner planet remains constant as there is very little gas left in its vicinity to induce any migration. When the distance of close approach eventually becomes smaller than the mutual Hill radius, the eccentricities increase strongly and the system may become unstable. If disc depletion occurs rapidly enough before the planets come too close to each other, a stable system similar to our own Solar system may remain. Otherwise the orbits may become unstable and produce systems like υ And.