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

Details Molecular Evolution in Interstellar Clouds. I ---Ion Chemistry in Dense Clouds--- Molecular Evolution in Interstellar Clouds. I ---Ion Chemistry in Dense Clouds---

Oct 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979pthph..62..936s&link_type=abstract

Progress of Theoretical Physics, Vol. 62, No. 4, pp. 936-956

Physics

46

Scientific paper

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 (nH=105cm-8, T=30K ζH=10-18 s-1 per H atom), observed molecules are produced successfully and attain their steady-state abundances at t = ˜ 2 × 1016s, 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= ˜ 1016s, when most C atoms are consumed in forming CO molecules. The C/CO ratio is a good indicator of molecular evolution in dense clouds.

Affiliated with

Also associated with

No associations

Rating

Molecular Evolution in Interstellar Clouds. I ---Ion Chemistry in Dense Clouds--- does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Molecular Evolution in Interstellar Clouds. I ---Ion Chemistry in Dense Clouds---, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Molecular Evolution in Interstellar Clouds. I ---Ion Chemistry in Dense Clouds--- will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1388604