On the evolution of diffuse interstellar clouds

Details On the evolution of diffuse interstellar clouds On the evolution of diffuse interstellar clouds

Sep 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992mnras.258..377h&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 258, no. 2, Sept. 15, 1992, p. 377-383. Research suppor

Astronomy and Astrophysics

Astronomy

11

Interstellar Matter, Molecular Clouds, Molecular Diffusion, Radiative Transfer, Chemical Equilibrium, Galactic Evolution, Ortho Hydrogen, Para Hydrogen, Photodissociation

Scientific paper

Models of a diffuse interstellar cloud which illustrate the progression from largely atomic to molecular gas with increasing optical depth are modeled. The medium is assumed to evolve isobarically, and the time-dependent chemistry is followed with the aid of a library of about 500 reactions. The transfer of ultraviolet radiation in the absorption lines of H2 and CO is treated numerically, using a grid of approximately 300,000 points in the wavelength range 91-126 nm. The calculations show that the time required to form molecular hydrogen and carbon monoxide within the cloud is large compared with the probable cloud lifetime. It seems likely that at least a fraction of the H2 and CO which are observed in diffuse clouds has formed in dense clouds and has subsequently been mixed into the diffuse medium.

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