Migration and giant planet formation

Details Migration and giant planet formation Migration and giant planet formation

2004-03-24

arxiv.org/abs/astro-ph/0403574v1

Astron.Astrophys. 417 (2004) L25-L28

Astronomy and Astrophysics

Astrophysics

9 pages, 2 figures, published in A&A Letters

Scientific paper

10.1051/0004-6361:20040053

We extend the core-accretion model of giant gaseous planets by Pollack et al. (\cite{P96}) to include migration, disc evolution and gap formation. Starting with a core of a fraction of an Earth's mass located at 8 AU, we end our simulation with the onset of runaway gas accretion when the planet is at 5.5 AU 1 Myr later. This timescale is about a factor ten shorter than the one found by Pollack et al. (\cite{P96}) even though the disc was less massive initially and viscously evolving. Other initial conditions can lead to even shorter timescales. The reason for this speed-up is found to result from the fact that a moving planet does not deplete its feeding zone to the extend of a static planet. Thus, the uncomfortably long formation timescale associated with the core-accretion scenario can be considerably reduced and brought in much better agreement with the typical disc lifetimes inferred from observations of young circumstellar discs.

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