Dark cloud chemistry in initially H-rich regions

Abstract

The chemistry in dark regions of dense cores is explored as a function of the initial abundance ratio of H to H 2 , on the assumption that some cores form on a timescale and are younger than the time required for the H:H 2 ratio to attain its equilibrium value. Observational diagnostics of non-equilibrium values of the initial H:H 2 ratio are identified. In initially H-rich material, the abundances of OH, NH 3 , CN, and HNC are for some time higher than they are in initially H-poor material. In initially H-poor regions, the abundances of CO, species containing multiple carbon atoms in each molecule, and CS are larger for an (observationally significant) period than in initially H-rich material.