Observations of C-13 Isotopomers of HC3N and HC5N in TMC-1: Evidence for Isotopic Fractionation

Details Observations of C-13 Isotopomers of HC3N and HC5N in TMC-1: Evidence for Isotopic Fractionation Observations of C-13 Isotopomers of HC3N and HC5N in TMC-1: Evidence for Isotopic Fractionation

Aug 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997nsro.rept.....t&link_type=abstract

Technical Report, NRO-Rept.-442

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Carbon 13, Ultraviolet Radiation, Interstellar Radiation, Chemical Reactions, Fractionation, Acetylene, Isotopes, Carbon, Stellar Envelopes, Interstellar Matter, Abundance

Scientific paper

The carbon chain molecules are well known due to their large abundances in cold dark clouds (e.g. Benson & Myers; Suzuki et al.) and in some carbon-rich circumstellar envelopes (e.g. Jewell & Snyder; Sopka et al.; Fukasaku et al.). About 40 % of interstellar molecules are classified as carbon chain molecules. The study of these molecules is, therefore, important to understand chemical processes in space. Several formation mechanisms for the carbon chain molecules have been proposed. For example, Schiff & Bohme and Mitchell et al. proposed to explain the carbon chain growth by C2 units: C2H2(+) or C2H2. On the other hand, Suzuki proposed that C(+), which was produced by interstellar ultraviolet radiation, plays an important role for the carbon chain formation. Given these possibilities, we have been obtaining observational information on the mechanism of carbon chain formation. One observational approach is to study C-13 isotopic fractionation in the carbon chain molecules. If C-13 isotopic fractionation is found, we can discuss the mechanisms of fractionation and the origin of the fractionated carbon. Such discussions are quite useful to study formation mechanisms.

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