The combined role of ionization and supernova explosions in the destruction of molecular clouds

Details The combined role of ionization and supernova explosions in the destruction of molecular clouds The combined role of ionization and supernova explosions in the destruction of molecular clouds

Jun 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989a%26a...216..207y&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 216, no. 1-2, June 1989, p. 207-214. Research supported by Max-Planck-Institut

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32

Computational Astrophysics, Gas Ionization, H Ii Regions, Molecular Clouds, Supernovae, Astronomical Models, Galactic Evolution, O Stars, Star Formation Rate

Scientific paper

Two-dimensional axially symmetric calculations of the evolution of a molecular cloud containing a single O star embedded at varying depths within the cloud were performed. The O star first produces an expanding champagne-type H II region and subsequently explodes as a type II supernova. The calculations cover a region extending at least 60 pc into the intercloud medium and display the complete evolution of the H II region on this scale. During the champagne phases, the ionizing radiation of the 0 star results in the escape of cloud material at the rate of 3-5 10-3 Msun yr-1. This rate is in agreement with that obtained in earlier work. For stars deeply embedded in the cloud (greater-than or equivalent to 3 pc) another feature is found -- a long-lived high-density brim which to some extent collimates the champagne flow. A supernova occurring in the cavity left by the H II region results in relatively little additional mass loss. The outward-moving supernova shock compresses most of the previously ejected cloud material into a thin shell, which appears to be Rayleigh-Taylor unstable. Ultimately, the cavity left by the passage of the supernova blast wave is refilled by cloud material, most of which remains bound to the cloud.

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