Planet Migration in Self-Gravitating Discs: Survival of Planets

Abstract

We carry out three-dimensional SPH simulations to study whether planets can survive in self-gravitating protoplanetary discs. The discs modelled here use a cooling prescription that mimics a real disc which is only gravitationally unstable in the outer regions. We do this by modelling the cooling using a simplified method such that the cooling time in the outer parts of the disc is shorter than in the inner regions, as expected in real discs. We find that both giant (> M_Sat) and low mass (< M_Nep) planets initially migrate inwards very rapidly, but are able to slow down in the inner gravitationally stable regions of the disc without needing to open up a gap. This is in contrast to previous studies where the cooling was modelled in a more simplified manner where regardless of mass, the planets were unable to slow down their inward migration. This shows the important effect the thermodynamics has on planet migration. In a broader context, these results show that planets that form in the early stages of the discs' evolution, when they are still quite massive and self-gravitating, can survive.

13 pages, 14 figures, accepted for publication in MNRAS

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• Orbital Migration of Protoplanets in a Marginally Gravitationally Unstable Disk. II. Migration, Merging, and Ejection
• The link between infall location, early disc size, and the fraction of self-gravitationally fragmenting discs
• DIPSY: A new Disc Instability Population SYnthesis, II. The Populations of Companions Formed Through Disc Instability
• Calibrated Gas Accretion and Orbital Migration of Protoplanets in 1D Disc Models
• Continuing to Hide Signatures of Gravitational Instability in Protoplanetary Discs with Planets
• DIPSY: A new Disc Instability Population SYnthesis, I. Modeling, evolution of individual systems, and tests
• Secular Spin-orbit Resonances of Black Hole Binaries in AGN Disks
• Gravitational instability in planet-forming discs