Research on the Early History of the Solar System

The evolution of a dissipating turbulently viscous disk of gas and dust formed during the collapse of an interstellar cloud fragment and how it relates to the early history of the solar system is discussed. Results from calculations on modelling the inner parts of the primitive solar nebula subject to the assumption of a steady inward flow are given. Other calculations are reviewed which simulate the accretion of a star from an accretion disk. Scenarios for the evolution of the primitive solar nebula and the formation of the Moon as a result of a major collision with the protoearth are described.