CN and HCN in Dense Interstellar Clouds
Abstract
We present a theoretical investigation of CN and HCN molecule formation in dense interstellar clouds. We study the gas-phase CN and HCN production efficiencies from the outer photon-dominated regions (PDRs) into the opaque cosmic-ray dominated cores. We calculate the equilibrium densities of CN and HCN, and of the associated species C+, C, and CO, as functions of the far-ultraviolet (FUV) optical depth. We consider isothermal gas at 50 K, with hydrogen particle densities from 102 to 106 cm-3. We study clouds that are exposed to FUV fields with intensities 20 to 2*105 times the mean interstellar FUV intensity. We assume cosmic-ray H2 ionization rates ranging from 5*10-17 s-1, to an enhanced value of 5*10-16 s-1. We also examine the sensitivity of the density profiles to the gas-phase sulfur abundance.
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