University of Cambridge > Talks.cam > DAMTP Astrophysics Seminar > Unveiling the role of dust on planetary migration

Unveiling the role of dust on planetary migration

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If you have a question about this talk, please contact Cleo Loi.

Gas and dust are essential components of protoplanetary disks, actively participating in the formation of planetesimals and planetary bodies. The gravity of planetary embryos perturbs the disk which, in turn, reacts producing gravitational feedback onto the nascent planets. This feedback has the potential of changing the planets’ orbits, leading to a process known as planetary migration. The characterization of this migration requires detailed calculations of the global disk structure and detailed physical models. For example, the headwind exerted by a sub-Keplerian gas flow onto dust particles produces a mutual radial drift which, combined with planet torques, may have a significant effect on the resulting local mass distribution of the disk. This dust torque could—depending on the dust-to-gas mass ratio, the particle-size distribution, and the mass of the embryos—modify the orbit of the nascent planets. In this talk, I will present recent results related to torques induced by scattered pebble-flows in protoplanetary disks, obtained with the new multifluid version of the publicly available code FARGO3D .

This talk is part of the DAMTP Astrophysics Seminar series.

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