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Review of disc-planet interactions

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The interactions of a young planet with its surrounding gaseous disc are likely responsible for the properties of many of the observed extra-solar planets. The masses of these planets are determined by tidal truncation or gas dispersal. Their orbital radii are determined in part by planet migration. Disc-planet interactions may play a role in exciting the orbital eccentricities of planets. A major uncertainty in evaluating these interactions is the physical state of the disc about which we have little direct observational evidence. The nature of disc turbulence and structure of the disc can have an important influence on the outcome of the interactions. Understanding how these interactions affect the planet formation process is a major challenge.

This talk is part of the Isaac Newton Institute Seminar Series series.

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