How Massive Are Population III Stars?

Details How Massive Are Population III Stars? How Massive Are Population III Stars?

Dec 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999sf99.proc...28n&link_type=abstract

Star Formation 1999, Proceedings of Star Formation 1999, held in Nagoya, Japan, June 21 - 25, 1999, Editor: T. Nakamoto, Nobeyam

Computer Science

Scientific paper

We study the gravitational contraction and fragmentation of filamentary primordial gas clouds by means of one-dimensional (1D) and two-dimensional (2D) hydrodynamical simulations. The cloud evolution is computed from the central proton density nc 102 - 106 cm-3 up to 1011-12 cm-3. From the 1D simulations, it is found that the radial contraction decelerates after the central density reaches 104 cm-3, beyond which the LTE populations are achieved for the rotational levels of hydrogen molecules. When the central density reaches 1011-12 cm-3, the cloud becomes optically thick to the H2 lines. Therefore, the radial contraction almost stops at that stage. From the 2D simulations, it is found that the fragmentation takes place during the stages at which 104 cm-3 < nc < 1011-12 cm-3 because the radial contraction becomes slower. The fragment mass depends on the initial model parameters such as the central density and temperature. For the higher initial temperature and higher initial density, the fragment mass is lower. Then, the maximum and minimum masses are estimated as 103 Modot and 1 2 Modot, respectively. If one fragment collapses into one star, then the masses of the first stars are expected to range from 1-2 Modot to 103 Modot, which are low-mass deficient compared to the Pop I stars. The effect of HD cooling is also discussed.

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