The dynamical evolution of massive protostellar clouds

Details The dynamical evolution of massive protostellar clouds The dynamical evolution of massive protostellar clouds

Jan 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977a%26a....54..183y&link_type=abstract

Astronomy and Astrophysics, vol. 54, no. 1, Jan. 1977, p. 183-194. Research supported by the Deutsche Forschungsgemeinschaft.

Astronomy and Astrophysics

Astrophysics

191

B Stars, O Stars, Protostars, Stellar Evolution, Abundance, Cosmic Dust, H Ii Regions, Heavy Elements, Interstellar Matter, Photosphere, Statistical Analysis, Stellar Luminosity, Winter

Scientific paper

The dynamic evolution of a protostellar cloud massive enough to form an OB star is investigated by calculating the hydrodynamic evolution of a spherically symmetric cloud envelope consisting of gas and dust. The dust is assumed to be composed of unequal amounts of ice-coated and pure spherical graphite grains. Results obtained for clouds of 50 and 150 solar masses are discussed in detail. In the discussion, attention is given to the usual initial stages of collapse, the structure of the protostellar cocoon shortly after its formation, the behavior of the outer envelope, and mass accretion onto the protostar. The formation of an initial H II region is examined, the IR appearance of the protostar during its late evolutionary stages is estimated qualitatively, and the efficiency of star formation is found to be rather low. The photospheric heavy-element abundance of the ZAMS star is briefly discussed along with oscillations of the inner cocoon and effects of increased dust opacity.

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