Modeling the chemistry of the dense interstellar clouds. I - Observational constraints for the chemistry

Details Modeling the chemistry of the dense interstellar clouds. I - Observational constraints for the chemistry Modeling the chemistry of the dense interstellar clouds. I - Observational constraints for the chemistry

May 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...354..504f&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 354, May 10, 1990, p. 504-512.

Astronomy and Astrophysics

Astrophysics

20

Astronomical Models, Interstellar Chemistry, Interstellar Matter, Molecular Clouds, Ammonia, Carbon Monoxide, Formaldehyde, Line Spectra, Molecular Spectra, Ultraviolet Radiation

Scientific paper

A search for correlations arising from molecular line data is made in order to place constraints on the chemical models of interstellar clouds. At 10 to the 21st H2/sq cm, N(CO) for dark clouds is a factor of six greater than the value for diffuse clouds. This implies that the strength of the UV radiation field where CO shields itself from dissociation is about one-half the strength of the average Galactic field. The dark cloud data indicate that the abundance of CO continues to increase with A(V) for directions with A(V) of 4 mag or less, although less steeply with N(H2) than for diffuse clouds. For H2CO, a quadratic relationship is obtained in plots versus H2 column density. The data suggest a possible turnover at the highest values for A(V). NH3 shows no correlation with H2, C(O-18), HC3N, or HC5N; a strong correlation is found between HC5N and HC3N, indicating a chemical link between the cyanopolyynes.

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