Statistics – Computation
Scientific paper
Oct 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984stfm.work...63y&link_type=abstract
In Royal Observatory Star Formation Workshop p 63-82 (SEE N85-12809 03-88)
Statistics
Computation
17
Protostars, Stellar Envelopes, Stellar Evolution, Stellar Models, Stellar Spectra, Hydrodynamic Equations, Molecular Clouds, Radiation Transport
Scientific paper
Investigations of protostars using model fitting techniques, and construction of model grids is reviewed. An approach based on numerical hydrodynamical evolution equations coupled with radiation transport is outlined. The evolution of the envelope, its density and velocity structure are determined by physical equations, but to reduce computational complexity, assumptions are made. Boundary conditions, initial starting conditions, and detailed knowledge of dust properties are, however, needed. Such evolutionary calculations cannot be repeated for a wide range of parameters, and it is difficult to judge whether the final results depend sensitively on the assumptions made. If used with the first two approaches, though, the method provides valuable insight into the star formation process. The evolution and collapse of a 10 and 150M cloud are analyzed.
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