I. Cherchneff et al., Dust formation in carbon-rich Wolf-Rayet stars I. Chemistry of small carbon clusters and silicon species, ASTRON ASTR, 357(2), 2000, pp. 572-580
The formation of small carbon chains and molecular precursors to silicon ca
rbide grains is investigated in the hot, hostile environment of carbon-rich
Wolf-Rayet (WC) winds. We consider only WC stars which produce dust on a c
ontinuous basis and develop for the first time non-equilibrium, chemical ki
netic routes to nucleating dust precursors in the outflow. These can be use
d to calculate quantitatively the yield of such dust precursors for various
outflow scenarios. Because WC stars have lost all their hydrogen in the WN
phase, the chemical processes used in the model involve a pure helium, car
bon, oxygen, silicon and sulphur chemistry which resembles that encountered
in graphite or metal vaporization experiments in the laboratory. We derive
abundances for small linear carbon clusters up to C-6 and silicon-bearing
species for various wind parameters and conclude that high-density regions
in the form of clumps or discs are of paramount importance to the formation
of dust in WC stars.