Models of Photodissociated Regions

Details Models of Photodissociated Regions Models of Photodissociated Regions

Jan 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998baas...30..766d&link_type=abstract

American Astronomical Society Meeting, 191, #129.07

Astronomy and Astrophysics

Astronomy

Scientific paper

Photodissociated regions (PDRs) are created within molecular clouds by the radiation field of newly formed stars. Large amounts of photodissociated and ionized material are produced in the neighborhood of OB stars by the strong stellar FUV fluxes, while intermediate mass stars form photodissociated regions of moderate size. The expansion of the H II region in the PDR reduces the mass of H I around OB stars, ionizing it in time scales that depend on the density of the gas and stellar flux. The expansion of the ionized region drives a strong shock that advances ahead of the ionization front; the dissociation front produces only a weak shock driven by the pressure difference between the molecular and atomic gas. Numerical models for the evolution of the composite H II + PDR regions, in different media, are presented. The contribution to the destruction of the molecular clouds by PDRs is also discussed.

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