2004/12/16 by Y. Alibert, Yann Alibert, C. Mordasini +5 · 17 citations
Physics and Astronomy · #Astro and Planetary Science #Astrophysics and Star Formation Studies #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1051/0004-6361:20042032
published as Astron.Astrophys.434:343-353,2005 · Accepted in Astronomy & Astrophysics
arxiv created 2004/12/16 · openalex publication_date 2005/04/01 · arxiv updated 2011/05/05 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/01
We present a new model of giant planet formation that extends the core-accretion model of Pollack et al. (1996, Icarus, 124, 62) to include migration, disc evolution and gap formation. We show that taking these effects into account can lead to much more rapid formation of giant planets, making it compatible with the typical disc lifetimes inferred from observations of young circumstellar discs. This speed up is due to the fact that migration prevents the severe depletion of the feeding zone as observed in in situ calculations. Hence, the growing planet is never isolated and it can reach cross-over mass on a much shorter timescale. To illustrate the range of planets that can form in our model, we describe a set of simulations in which we have varied some of the initial parameters and compare the final masses and semi-major axes with those inferred from observed extra-solar planets.