Models of Uranus' interior and magnetic field

Our understanding of Uranus' interior structure comes from the results of theoretical models. In this chapter, the methods for computing such models are reviewed. The various physical assumptions employed are discussed and their strengths and weaknesses are assessed. The accretion theory of the formation of the planets is summarized and the implications for the structure and composition of Uranus are presented. The results of the most recent modeling efforts are then discussed. The implications of these model results are examined for their bearing on three important questions. First, the anomalously low internal heat source of the planet compared to its insolation, second, the strongly tilted dipole of the magnetic field and finally the chemistry of Uranus' atmosphere and deep interior. The implications of these models for theories of the formation of Uranus are discussed. -from Authors