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Fragmentation in turbulent primordial gas

Published online by Cambridge University Press:  27 April 2011

S. C. O. Glover ,
P. C. Clark ,
R. S. Klessen  and
V. Bromm
S. C. O. Glover
Affiliation:
Institut für Theoretische Astrophysik, Zentrum für Astronomie der Universität Heidelberg, Albert-Ueberle-Str. 2, 69120 Heidelberg, Germany
P. C. Clark
Affiliation:
Institut für Theoretische Astrophysik, Zentrum für Astronomie der Universität Heidelberg, Albert-Ueberle-Str. 2, 69120 Heidelberg, Germany
R. S. Klessen
Affiliation:
Institut für Theoretische Astrophysik, Zentrum für Astronomie der Universität Heidelberg, Albert-Ueberle-Str. 2, 69120 Heidelberg, Germany
V. Bromm
Affiliation:
Department of Astronomy, University of Texas, Austin, TX 78712
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Abstract

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We report results from numerical simulations of star formation in the early universe that focus on the role of subsonic turbulence, and investigate whether it can induce fragmentation of the gas. We find that dense primordial gas is highly susceptible to fragmentation, even for rms turbulent velocity dispersions as low as 20% of the initial sound speed. The resulting fragments cover over two orders of magnitude in mass, ranging from ~0.1 M⊙ to ~40 M⊙. However, our results suggest that the details of the fragmentation depend on the local properties of the turbulent velocity field and hence we expect considerable variations in the resulting stellar mass spectrum in different halos.

Keywords

stars: formation – galaxies: formation – cosmology: theory
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S270: Computational Star Formation , May 2010 , pp. 499 - 502
Copyright
Copyright © International Astronomical Union 2011

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