Calculations of the condensation path of a gas of solar composition were made taking into account barriers to the homogeneous nucleation of the condensed phase. Our results indicate that the primordial dust had much more variability of form and composition than has been previously assumed. A mechanism is deduced for the formation of meteoritic chondrules at temperatures and pressures which are much lower and more plausible than those postulated by WOOD. The supersaturation of the gas phase also leads to much higher concentrations of FeO in the silicate condensate than has been calculated assuming equilibrium condensation, with the concentration of FeO in the condensate being a variable which is dependent on the conditions of condensation. This is consistent with observations of variability of the composition of FeO between different classes of meteorites and between different silicate crystallites in the unequilibrated chondrites. Our calculations raise the possibility that some of the properties of meteorites which have been ascribed to a complex sequence of processes are in reality of a much simpler and more primitive origin associated with the primary condensation.