Model calculations for diffuse molecular clouds

Details Model calculations for diffuse molecular clouds Model calculations for diffuse molecular clouds

Oct 1974

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1974apj...193...73g&link_type=abstract

Astrophysical Journal, vol. 193, Oct. 1, 1974, pt. 1, p. 73-91.

Astronomy and Astrophysics

Astrophysics

112

Abundance, Astronomical Models, Hydrogen Clouds, Interstellar Gas, Molecular Gases, Density Distribution, Fine Structure, Interstellar Extinction, Oao 3, Radiative Transfer, Steady State

Scientific paper

A local steady-state isobaric model of the interstellar clouds is developed and applied to the OAO-3 observations. The model allows for cooling by C II fine-structure transitions and for inhomogeneities resulting from attenuations in the external radiations which heat the cloud constituents. Factors affecting the thermal properties of the clouds are emphasized; these include H and H2 balance, interstellar grain heating, electron density, and calcium equilibrium. The thermodynamic consequences of the attenuation of the ultraviolet interstellar radiation field are studied. The effect of varying the most important parameters and their allowed ranges is considered. Results indicate that the model is capable of reproducing the H2 fractional abundances and kinetic temperatures observed by OAO-3.

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