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Planetary migration in Solar System formation

Abstract : Planetary migration seems to be unavoidable during planet formation in protoplanetary disks. Gravitational interactions between the planet embryos and the gas disk make the angular momentum of the embryo decrease, so that it spirals towards the central star. As the migration timescale is shorter than the disk life time, no planet should survive (chapters 1 and 2). In this thesis, we try to find mechanisms that prevent or slow down migration.

In chapter 3, we show that a jump in the gas disk density stops migration and acts like a planet trap. Trapped there, a massive solid core may accrete a gaseous atmosphere and give birth to a giant planet. The planet is then massive enough to repel the gas and open a gap around its orbit. Through analysis of computer simulations, we enlighten the role of pressure effects in this process in chapter 4 ; a new generalized gap opening criterion is derived. After the presentation of a new, reliable and performing algorithm for numerical simulations in chapter 5, we use it in chapter 6 to study the migration of a giant planet and its influence on the disk evolution. The formation of a cavity appears to be less easy than previously expected, but we find a way of preventing migration. Last, in chapter 7, we focus on the case of Jupiter and Saturn, and we find in which conditions the interactions between both planets prevent their migration.
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Contributor : Aurélien Crida <>
Submitted on : Tuesday, October 14, 2008 - 1:00:08 PM
Last modification on : Wednesday, October 14, 2020 - 4:23:37 AM
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  • HAL Id : tel-00330414, version 1



Aurélien Crida. Planetary migration in Solar System formation. Astrophysics [astro-ph]. Université Nice Sophia Antipolis, 2006. English. ⟨tel-00330414⟩



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