Chemical condensation in the outflowing matter from the proto-sun and its application to meteorites

A novel model for solar nebula is proposed which is based on the observations of nebular disks around young solar-type stars in their T Tauri phase and the evidence that these disks formed from the material condensed from the outflowing gases from these stars. The model makes it possible to calculate the mass and the angular momentum. From these, parameters and the known photospheric temperature of T Tauri stars, the characteristic features of the nebula (such as radial extent, thickness, and temperature and pressure profiles) can be calculated. The model accounts very well for meteoritic mineralogy. It is suggested that chemical condensation took place in the outflowing matter from the protosun and that the solar nebula formed from this condensed material. The model also accounts for the formation of ices in the outer solar system and for planetary composition.