Molecular Evolution in Interstellar Clouds. I : Ion Chemistry in Dense Clouds

概要

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Molecular abundances are calculated time-dependently using a chemical scheme which is constructed to represent the evolutional feature of all molecules containing up to 2 heavy atoms (C, N, O, S and Si) and consisted of the surface recombination of hydrogen on grains and 2884 gas phase reactions of 234 species. For the model adopted (n_H=10^5 cm^<-3>, T=30 K, ζ_H=10^<-18> s^<-1> per H atom), observed molecules are produced successfully and attain their steady-state abundances at t=〜2×10^<16>s, which is longer than the evolutional time scale of dense clouds. Molecules containing carbon (except carbon in C-O bond) have peak abundances at t=〜10^<15>s, when most C atoms are consumed in forming CO molecules. The C/CO ratio is a good indicator of molecular evolution in dense clouds.
理論物理学刊行会の論文
1979-10-25