Radiatively driven dust-bounded implosions - Formation and stability of dense globules

Details Radiatively driven dust-bounded implosions - Formation and stability of dense globules Radiatively driven dust-bounded implosions - Formation and stability of dense globules

Jul 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...282..178s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 282, July 1, 1984, p. 178-190. Research supported by the U.S. Department of

Astronomy and Astrophysics

Astrophysics

22

Flow Stability, Hydrogen Clouds, Interstellar Matter, Molecular Clouds, Radiative Transfer, Stellar Evolution, Astronomical Models, Cosmic Dust, Gas Density, Hydrodynamic Equations

Scientific paper

Two-phase radiation hydrodynamic calculations of the collapse of dusty globules illuminated by an external radiation source are presented. Anisotropic scattering by the dust grains and momentum coupling between the dust and gas phases are included. THe present work is a continuation of earlier work by Sandford, Whitaker, and Klein. Two models are presented, an optically thin case and a 1-solar-mass optically thick globule. Radiation pressure acts on the dust, which moves with subsonic velocity, and in both cases the ionization front eventually becomes dust bounded. The presence of dust lengthens the time scale for globular compression by a factor of 3 for the optically thin case and dust extinction limits the speed with which the ionization front moves into the cloud. Results for the optically thick model indicate that the globule survives long enough for self-gravity to act, resulting in the formation of low mass stars or long-lived, stable dark globules.

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