H I: A Chemical Tracer of Turbulent Diffusion in Molecular Clouds

Details H I: A Chemical Tracer of Turbulent Diffusion in Molecular Clouds H I: A Chemical Tracer of Turbulent Diffusion in Molecular Clouds

Jul 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002apj...573l.119w&link_type=abstract

The Astrophysical Journal, Volume 573, Issue 2, pp. L119-L122.

Astronomy and Astrophysics

Astronomy

21

Diffusion, Ism: Abundances, Ism: Clouds, Ism: Molecules, Molecular Processes, Turbulence

Scientific paper

Turbulence is widespread in the interstellar medium, and turbulent diffusion has been suggested as a means of accounting for the lower than expected O2 abundance observed in molecular clouds by the Submillimeter Wave Astronomy Satellite. Here we present the results of new chemical models of clouds incorporating turbulent diffusion, together with gas-grain interactions and H2 and CO self-shielding. We find H I to be a very sensitive tracer of the diffusion process, with H I/H2 larger in the interior than predicted by static models. Our model may explain observations of H I/H2 in cold cores. The model results for other species, e.g., O, O2, H2O, C, and CO, are also consistent with available observations. This work demonstrates the potential importance of chemical studies in the elucidation of turbulent processes in the interstellar medium.

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