Abstract

Jupiter and Saturn have been observed for thousands of years, but their genesis remains uncertain. This talk will briefly review the theories of their formation that have come and gone, and those that dominate the field today. Results will be presented from recent three-dimensional self-gravitating radiation hydrodynamical models of gas accretion on to proto-giant planets performed with the smoothed particle hydrodynamics (SPH) method. The properties of their co-evolving circumplanetary discs (where present) will also be discussed. The discovery of a diverse population of exoplanets has forced theories to adapt in order to explain the array of properties that are now being observed. One mechanism seen as key in the formation of Hot Jupiters is that of migration, without which current formation theories fail. On going work to model the migration of giant planets will be presented.