Carbon chemistry in dense molecular clouds: Theory and observational constraints

Details Carbon chemistry in dense molecular clouds: Theory and observational constraints Carbon chemistry in dense molecular clouds: Theory and observational constraints

Apr 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990nascp3061..159b&link_type=abstract

In NASA, Ames Research Center, Carbon in the Galaxy: Studies from Earth and Space p 159-179 (SEE N90-27562 21-88)

Astronomy and Astrophysics

Astrophysics

Carbon, Interstellar Chemistry, Molecular Clouds, Planetary Evolution, Stars, Stellar Evolution, Vapor Phases, Abundance, Astronomical Models, Astrophysics, Failure, Inventories, Low Temperature Environments, Mathematical Models, Millimeter Waves, Spectra, Submillimeter Waves, Surveys

Scientific paper

For the most part, gas phase models of the chemistry of dense molecular clouds predict the abundances of simple species rather well. However, for larger molecules and even for small systems rich in carbon these models often fail spectacularly. Researchers present a brief review of the basic assumptions and results of large scale modeling of the carbon chemistry in dense molecular clouds. Particular attention is to the influence of the gas phase C/O ratio in molecular clouds, and the likely role grains play in maintaining this ratio as clouds evolve from initially diffuse objects to denser cores with associated stellar and planetary formation. Recent spectral line surveys at centimeter and millimeter wavelengths along with selected observations in the submillimeter have now produced an accurate inventory of the gas phase carbon budget in several different types of molecular clouds, though gaps in our knowledge clearly remain. The constraints these observations place on theoretical models of interstellar chemistry can be used to gain insights into why the models fail, and show also which neglected processes must be included in more complete analyses. Looking toward the future, larger molecules are especially difficult to study both experimentally and theoretically in such dense, cold regions, and some new methods are therefore outlined which may ultimately push the detectability of small carbon chains and rings to much heavier species.

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