Volume 552, April 2013
|Number of page(s)||14|
|Section||Planets and planetary systems|
|Published online||26 March 2013|
Nebular gas drag and planetary accretion with eccentric high-mass planets⋆
1 Univ. Estadual Paulista – UNESP, Grupo de Dinâmica Orbital & Planetologia, Guaratinguetá, , CEP 12516-410, SP, Brazil
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2 Univ. Estadual Paulista – UNESP, DCCE – IBILCE, São Jose do Rio Preto, 01405900 SP, Brazil
Received: 12 December 2011
Accepted: 23 January 2013
Aims. We investigate the dynamics of pebbles immersed in a gas disk interacting with a planet on an eccentric orbit. The model has a prescribed gap in the disk around the location of the planetary orbit, as is expected for a giant planet with a mass in the range of 0.1–1 Jupiter masses. The pebbles with sizes in the range of 1 cm to 3 m are placed in a ring outside of the giant planet orbit at distances between 10 and 30 planetary Hill radii. The process of the accumulation of pebbles closer to the gap edge, its possible implication for the planetary accretion, and the importance of the mass and the eccentricity of the planet in this process are the motivations behind the present contribution.
Methods. We used the Bulirsch-Stoer numerical algorithm, which is computationally consistent for close approaches, to integrate the Newtonian equations of the planar (2D), elliptical restricted three-body problem. The angular velocity of the gas disk was determined by the appropriate balance between the gravity, centrifugal, and pressure forces, such that it is sub-Keplerian in regions with a negative radial pressure gradient and super-Keplerian where the radial pressure gradient is positive.
Results. The results show that there are no trappings in the 1:1 resonance around the L4 and L5 Lagrangian points for very low planetary eccentricities (e2 < 0.07). The trappings in exterior resonances, in the majority of cases, are because the angular velocity of the disk is super-Keplerian in the gap disk outside of the planetary orbit and because the inward drift is stopped. Furthermore, the semi-major axis location of such trappings depends on the gas pressure profile of the gap (depth) and is a = 1.2 for a planet of 1 MJ. A planet on an eccentric orbit interacts with the pebble layer formed by these resonances. Collisions occur and become important for planetary eccentricity near the present value of Jupiter (e2 = 0.05). The maximum rate of the collisions onto a planet of 0.1 MJ occurs when the pebble size is 37.5 cm ≤ s < 75 cm; for a planet with the mass of Jupiter, it is15 cm ≤ s < 30 cm. The accretion stops when the pebble size is less than 2 cm and the gas drag dominates the motion.
Key words: planets and satellites: formation / minor planets, asteroids: general / accretion, accretion disks
Appendices are available in electronic form at http://www.aanda.org
© ESO, 2013
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