Formation of the solar system.

The overall evolution of the solar system is discussed in terms of what is called the Kyoto model. Starting from the formation of the solar nebula, a multistep process is followed in detail, including growth and sedimentation of dust grains in the nebula, formation of planetesimals due to fragmentation of a dust layer, radial migration and accumulation of planetesimals to form large bodies, and the dissipation of the solar nebula. The thermal history of the early earth and the formation of its core and mantle structures are discussed, and the origin of satellites and rings is also considered. The importance of the interactions between solid bodies and the gas of the solar nebula in determining the various stages of the evolution of the solar system is stressed.