The masses of Population III stars

Details The masses of Population III stars The masses of Population III stars

Jul 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989mnras.239..371d&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 239, July 15, 1989, p. 371-380. Research supported by C

Astronomy and Astrophysics

Astronomy

20

Protostars, Star Formation, Stellar Mass, Fragmentation, Gravitational Collapse, Molecular Clouds, Stellar Models, Supermassive Stars

Scientific paper

The formation of Population III protostars is examined, validating the suggestion of De Araujo and Opher (1988) that the persistance of fluctuations of masses of about 10-1000 solar masses after the recombination era may be important in the fragmentation of massive clouds involved in the formation of Population III stars. The present analysis assumes that nonnegligible density perturbations are possible at the start of the collapse, and it employs the Gott and Rees (1975) density perturbation spectrum at the recombination era. It is found that a mass of 500 solar masses oscillates two times before collapsing, and that a mass of 50 solar masses oscillates seven times before collapsing.

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