Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 1981
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981mnras.197.1021c&link_type=abstract
Monthly Notices of the Royal Astronomical Society, vol. 197, Dec. 1981, p. 1021-1029.
Astronomy and Astrophysics
Astronomy
69
Helium, Hydrogen Clouds, Metallic Stars, Stellar Mass, Stellar Models, Abundance, Big Bang Cosmology, Free Fall, Nuclear Fusion, Optical Thickness, Prediction Analysis Techniques
Scientific paper
The temperature of a cloud of hydrogen-helium gas uncontaminated by metals is followed from postrecombination conditions to hydrogen ionization, assuming the collapse occurs on a free-fall time-scale. Four characteristic masses can be identified: 10 to the 6th solar masses for a sufficiently hot cloud to allow H2 to form; 20 solar masses at H2 dissociation; 0.5 solar mass at optical depth unity; and 0.06 solar mass at H ionization. The initial cloud is of low enough density (approximately 10,000/cu cm) that stellar winds will prevent stars heavier than 100 solar masses from forming. The characteristic masses 0.06 and 0.5 solar mass are found in environments with such high density (10 to the -2nd and 10 to the -8th g/cu cm, respectively) that they are identified with a protostellar inner and outer core; they will continue to accrete material for a minimum stellar mass of a few solar masses. A metal production yield of 10%, combined with the minimum metal abundance for ordinary stars, implies that the zero metal stars made up at most 10 to the -4th of the gas mass of the universe.
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