A survey of CCS, HC3N, HC5N, and NH3 toward dark cloud cores and their production chemistry

Details A survey of CCS, HC3N, HC5N, and NH3 toward dark cloud cores and their production chemistry A survey of CCS, HC3N, HC5N, and NH3 toward dark cloud cores and their production chemistry

Jun 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...392..551s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 392, no. 2, June 20, 1992, p. 551-570. Research supported by Morino Science

Astronomy and Astrophysics

Astronomy

173

Interstellar Chemistry, Molecular Clouds, Radio Astronomy, Star Formation, Abundance, Ammonia, Stellar Evolution, Stellar Mass

Scientific paper

Survey observations of CCS, HC3N, HC5N, and NH3 were carried out toward 49 dark cloud cores to examine the existence of a systematic relation between the chemical evolution and the physical evolution of dark clouds. The CCS radical was revealed to be abundant in cold and quiescent dark cloud cores, while it is much less abundant in star-forming regions. The column density of CCS shows a good positive correlation with those of HC3N and HC5N, indicating that the production chemistry of CCS is closely related to those of other carbon-chain molecules in dark clouds. On the other hand, the column density of CCS shows no correlation with that of NH3; NH3 tends to be abundant in star-forming regions. A possible chemical model for the production of CnS (n = 1-3) is proposed. Pseudo-time-dependent calculations based on the proposed model show that the calculated abundance of CCS in the early stage of chemical evolution agrees mostly with the observed value in TMC-1. The relations among the observed column densities are qualitatively interpreted as an effect of chemical evolution of dark clouds on the basis of simulation of the molecular synthesis; carbon-chain molecules including CCS are abundant in the early stages of chemical evolution, whereas NH3 is abundant in the later stages.

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