EDP Sciences
Free access
Volume 388, Number 2, June III 2002
Page(s) 615 - 631
Section Formation and evolution of planetary systems
DOI http://dx.doi.org/10.1051/0004-6361:20020490

A&A 388, 615-631 (2002)
DOI: 10.1051/0004-6361:20020490

Global $\vec{m} = \mathsf{1}$ modes and migration of protoplanetary cores in eccentric protoplanetary discs

J. C. B. Papaloizou

Astronomy Unit, Queen Mary, University of London, Mile End Rd, London E1 4NS, UK

(Received 29 November 2001 / Accepted 28 March 2002)

We calculate global m=1 modes with low pattern speed corresponding to introducing a finite eccentricity into a protoplanetary disc. We consider disc models which are either isolated or contain one or two protoplanets orbiting in an inner cavity. Global modes that are strongly coupled to inner protoplanets are found to have disc orbits which tend to have apsidal lines antialigned with respect to those of the inner protoplanets. Other modes corresponding to free disc modes may be global over a large range of length scales and accordingly be long lived. We consider the motion of a protoplanet in the earth mass range embedded in an eccentric disc and determine the equilibrium orbits which maintain fixed apsidal alignment with respect to the disc gas orbits. Equilibrium eccentricities are found to be comparable or possibly exceed the disc eccentricity. We then approximately calculate the tidal interaction with the disc in order to estimate the orbital migration rate. Results are found to deviate from the case of axisymmetric disc with near circular protoplanet orbit once eccentricities of protoplanet and disc orbits become comparable to the disc aspect ratio in magnitude. Aligned protoplanet orbits with very similar eccentricity to that of the gas disc are found to undergo litle eccentricity change while undergoing inward migration in general. However, for significantly larger orbital eccentricities, migration may be significantly reduced or even reverse from inwards to outwards. Thus the existence of global non circular motions in discs with radial excursions comparable to the semi-thickness may have important consequences for the migration and survival of protoplanetary cores in the earth mass range.

Key words: planetary systems: formation -- planetary systems -- planetary systems: protoplanetary disks -- stars: individual: Ups And

© ESO 2002