A model for diffuse interstellar clouds: Improvements to the theory of molecular hydrogen photodestruction and to the gas phase chemistry of carbon monoxide

Details A model for diffuse interstellar clouds: Improvements to the theory of molecular hydrogen photodestruction and to the gas phase chemistry of carbon monoxide A model for diffuse interstellar clouds: Improvements to the theory of molecular hydrogen photodestruction and to the gas phase chemistry of carbon monoxide

May 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979phdt.........4f&link_type=abstract

Ph.D. Thesis New York Univ., New York.

Astronomy and Astrophysics

Astrophysics

4

Carbon Monoxide, Cloud Physics, Environment Models, Gas Mixtures, Hydrogen, Photochemical Reactions, Astrophysics, Density (Mass/Volume), Ions, Satellite Observation, Temperature, Ultraviolet Radiation

Scientific paper

A theoretical model was developed to determine physical processes in conjunction with astrophysical observation. The calculations are based on isobaric, steady state, plane-parallel conditions. In the model, the cloud is illuminated by ultraviolet radiation from one side. The density and temperature of the gas are derived by involving energy conservation in terms of thermal balance. The abundance of approximately fifty atomic and molecular species, including important ionic species and simple carbon and oxygen bearing molecules was determined. Except for molecular hydrogen formation on dust grains, binary gas phase reactions are used to develop the chemistry of the model cloud. The theoretical model was appropriate for a particular range of physical parameters. The results of the steady state calculations were compared to ultraviolet observations, predominantly those with the Copernicus satellite.

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