Atomic to molecular hydrogen transition in interstellar clouds

Details Atomic to molecular hydrogen transition in interstellar clouds Atomic to molecular hydrogen transition in interstellar clouds

Jan 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979apj...227..466f&link_type=abstract

Astrophysical Journal, Part 1, vol. 227, Jan. 15, 1979, p. 466-473.

Astronomy and Astrophysics

Astrophysics

174

Atomic Spectra, Cosmic Dust, Interstellar Matter, Molecular Spectra, Radiative Transfer, Anisotropic Media, Electron Transitions, Granular Materials, Photodissociation, Ultraviolet Radiation

Scientific paper

The photodestruction of molecular hydrogen is reexamined in the context of recent observational data. Improvements in the theory of radiation transfer are made by using a more accurate self-shielding integral, treating anisotropic scattering by dust grains, and including photodissociation from excited rotational states. The total column density of hydrogen required to obtain 10% conversion decreases with a parameter, epsilon, the ratio of the formation rate to the destruction rate, as epsilon to the -m power, with m in the range 1.4-1.6. Satisfactory agreement with the data for thicker diffuse clouds is obtained for epsilon of about 0.00006.

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