Remaining gas-phase chemistry after cloud formation: Left: depleted gas element abundances after cloud formation. Right: molecular abundances of a selected number of species to demonstrate the differences between the oxygen-rich (blue) and carbon-rich cases. The underlaying atmosphere model is the same as in Fig. 1 with Teff = 2000 K, log(g) = 3.0 and initial solar abundances with the carbon adjusted according to the C/O ratio listed.
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