The first stars

Details The first stars The first stars

Nov 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983mnras.205..705s&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 205, Nov. 1983, p. 705-718.

Astronomy and Astrophysics

Astronomy

86

Interstellar Chemistry, Protostars, Stellar Evolution, Density Distribution, Interstellar Magnetic Fields, Plasma Clouds, Stellar Mass, Stellar Models, Thermal Instability

Scientific paper

Primordial clouds are likely to be remarkably uniform over stellar mass-scales in the absence of a pre-existing generation of stars. Thermal instability is found to occur during the collapse of a primordial cloud when the H2 abundance is rising and the H2 optical depth is of order unity. The e-folding rate for fluctuation growth exceeds the free-fall collapse rate by an order of magnitude. Large density fluctuations of mass-scale 0.1 solar mass arise in any collapsing cloud with metallicity not greater than 0.001 of the solar value. Gravitational instability ensures that many of the clumps coagulate to form protostars of masses extending up to the initial Jeans mass when the fluctuations develop, namely 100 solar masses. The primordial IMF should therefore have spanned the mass range from 0.1 to 100 solar masses, but may have been dominated by the more massive stars.

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