  Volatility-dependent fractionation of the rock-forming elements at high
temperatures is an early, widespread process during formation of the earliest
solids in protoplanetary disks. Equilibrium condensation calculations allow
prediction of the identities and compositions of mineral and liquid phases
coexisting with gas under presumed bulk chemical, pressure and temperature
conditions. A graphical survey of such results is presented for systems of
solar and non-solar bulk composition. Chemical equilibrium was approached to
varying degrees in the local regions where meteoritic chondrules, Ca-Al-rich
inclusions, matrix and other components formed. Early, repeated vapor-solid
cycling and homogenization, followed by hierarchical accretion in dust-rich
regions, is hypothesized for meteoritic inclusions. Disequilibrium chemical
effects appear to have been common at all temperatures, but increasingly so in
less refractory meteoritic components. Work is needed to better model
high-temperature solid solutions, indicators of these processes.
