Evolution of primoridal gas clouds

Details Evolution of primoridal gas clouds Evolution of primoridal gas clouds

Feb 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986ucsc.rept.....b&link_type=abstract

Final Technical Report, 15 Feb. 1984 - 28 Feb. 1986 California Univ., Santa Cruz.

Mathematics

Big Bang Cosmology, Mathematical Models, Molecular Clouds, Nuclear Fusion, Stellar Evolution, Stellar Mass, Abundance, Chemical Composition, Gravitational Effects, Hydrodynamics, Prediction Analysis Techniques, Radiation Pressure

Scientific paper

The dynamical, chemical, and thermal evolution of zero-metal gas clouds was modeled to study conditions of star formation in the early universe. Numerical results are given for the collapse of spherical clouds of mass 1000 and 50000 solar mass. Cooling by H2 lines and by photons emitted in H + e(-) yields H(-) = h nu maintains collapse until formation of an equilibrium protostellar core of mass 0.02 solar mass. The cooling by photons produced with H is essential for low mass star formation. If the cloud is fragmented, the evolution of the pieces is similar to that of the parent cloud, but the equilibrium core has larger density and mass.

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