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Giant planet formation by core accretion

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Dynamics of Discs and Planets

A review of the standard paradigm for giant planet formation, the core accretion theory is presented. First, an overview of the physical concepts used in this model is given, and results of classical core accretion models are shown. Then, various improvements and modifications to the original model are discussed. Such improvements are the inclusion of more realistic envelope opacities and solid accretion rates, of concurrent migration and disk evolution and of results of hydrodynamical simulations. The corresponding consequences are compared with the observational constraints given by the giant planets of our own solar system. Finally it is discussed how recently several groups have started to use core accretion models to understand the statistical properties of the quickly growing population of extrasolar giant planets.

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

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