Astronomy and Astrophysics – Astrophysics
Scientific paper
Jun 1977
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977a%26a....58..423y&link_type=abstract
Astronomy and Astrophysics, vol. 58, no. 3, June 1977, p. 423-432.
Astronomy and Astrophysics
Astrophysics
27
Gravitational Collapse, Infrared Spectra, Infrared Stars, Protostars, Stellar Evolution, Stellar Spectra, Angular Distribution, Density Distribution, H Ii Regions, Hydrodynamic Equations, Iterative Solution, Spatial Distribution, Stellar Envelopes, Stellar Models
Scientific paper
The detailed radiation transfer problem is solved numerically for spherically symmetric protostellar clouds during various stages of collapse. For these calculations the density distribution of the numerical hydrodynamic models presented by Yorke and Kruegel (1977) describing the birth of a massive star in a dense dusty cloud are used. At each radius the temperatures of various grain components, spectra and angular distribution of the radiation are solved simultaneously assuming radiative equilibrium. The spectral as well as the spatial distribution of the radiation flux over the entire disk is presented for a 50 solar-mass and a 150 solar-mass protostellar cloud at various evolutionary stages up to (but not including) the development of a compact H II region. In both cases the envelope surrounding the accreting protostar (which in later stages is a main sequence star) is always opaque to the stellar photons, and the resulting appearance is that of an extended infrared source.
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