The photoevaporation of interstellar clouds. I - Radiation-driven implosion

Details The photoevaporation of interstellar clouds. I - Radiation-driven implosion The photoevaporation of interstellar clouds. I - Radiation-driven implosion

Nov 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...346..735b&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 346, Nov. 15, 1989, p. 735-755. Research sponsored by NASA.

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H Ii Regions, Interstellar Matter, Molecular Clouds, Computational Astrophysics, Evaporation, Ionized Gases, Lyman Alpha Radiation, Radiation Distribution, Shock Fronts, Star Formation

Scientific paper

An approximate analytical solution is developed for the evolution of an interstellar neutral cloud exposed to the ionizing radiation of a newly formed star. The structure of a steady photoevaporation gas flow off a spherical ionization front is derived even for cases where the ionization front cannot be considered thin, and the downstream flow is not in ionization and thermal equilibrium. Under a wide range of conditions, the ionization front is approximately D-critical, and the ionized gas expands supersonically into the intercloud medium. The ionization front typically drives a strong shock into the initial cloud.

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