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A crucial phase during planetary growth is the migration when the planetarycore has been assembled, but the planet did not open a deep gap yet. Duringthis phase the planet is subject to fast type-I migration, which is mostlydirected inwards, and the planet can lose a significant fraction of itssemi-major axis. The duration of this phase is set by how long the planetaryenvelope needs to contract until it reaches a mass similar to the mass of theplanetary core, which is when runaway gas accretion can set in and the planetcan open a deeper gap in the disc, transitioning into the slower type-IImigration. This envelope contraction phase depends crucially on the planetarymass and on the opacity inside the planetary envelope. Here we study howdifferent opacity prescriptions influence the envelope contraction time and howthis in turn influences how far the planet migrates through the disc. We findwithin our simulations that the size distribution of the grains as well as thechemical composition of the grains crucially influences how far the planetmigrates before it can reach the runaway gas accretion phase. Grain sizedistributions with larger grain sizes result in less inward migration of thegrowing planet, due to faster gas accretion enabled by more efficient cooling.In addition, we find that planets forming in water poor environments cancontract their envelope faster and thus migrate less, implying that gas giantsforming in water poor environments might be located further away from theircentral star compared to gas giants forming in water rich environments. Futurestudies of planet formation that aim to investigate the chemical composition offormed gas giants need to take these effects self consistently into account.

Influence of grain sizes and composition on the contraction rates of planetary envelopes and on planetary migration