Abstract
In light of recent evidence that the oxygen to carbon ratio in Mira variables may be only slightly greater than 1.0, molecular dissociative equilibrium calculations are made using an O/C ratio of 1.03, O/H ratio of 10 –4 and Si/H ratio of |$4 \times 10^{-5}$| to determine the region of the P, T plane in which carbon is super-saturated and particle formation is possible. A system of equations describing the formation and growth of carbon particles throughout the temperature cycle of a variable star is solved for a gas undergoing temperature variations characteristic of those occurring in the atmospheres of Mira variables. The results show that a large number of extremely small particles will form and that the extinction due to these particles is several orders of magnitude greater than the expected atomic and molecular extinction.
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