H2O heating in molecular clouds - Line transfer and thermal balance in a warm dusty medium

Details H2O heating in molecular clouds - Line transfer and thermal balance in a warm dusty medium H2O heating in molecular clouds - Line transfer and thermal balance in a warm dusty medium

Dec 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...275..145t&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 275, Dec. 1, 1983, p. 145-162.

Mathematics

Probability

47

Gas Heating, Interstellar Matter, Molecular Clouds, Molecular Collisions, Radiative Heat Transfer, Water Vapor, Astronomical Models, Cosmic Rays, Gas Temperature, Heat Balance, Photoabsorption, Stellar Radiation

Scientific paper

An investigation is undertaken into the possibility of the heating of molecular gas through collisions with radiatively pumped H2O, in the context of the overall thermal balance of optically thick molecular clouds with embedded sources. In order to solve the line transfer equation, which includes warm dust grains, an extended method of escape probability approximation is developed in which the equilibrium gas temperature arises from the balance of heating by cosmic ray ionization of H2, and by collisions with warm dust grains and radiatively pumped H2O molecules against cooling by collisions with CO and C I. The equilibrium gas temperature for a given dust temperature strongly depends on the efficiency of the cooling species, and is therefore most sensitive to the cloud optical depth. It is less dependent, in decreasing order, on H2O abundance, gas density, and velocity dispersion.

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