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Assessing the influence of metallicity on fragmentation of proto-galactic gas

Published online by Cambridge University Press:  01 August 2006

Anne-Katharina Jappsen ,
Simon C. O. Glover ,
Ralf S. Klessen  and
Mordecai-Mark Mac Low
Anne-Katharina Jappsen
Affiliation:
Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, ON M5S 3H8, Canada email: [email protected] Astrophysikalisches Institut Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany email: [email protected]
Simon C. O. Glover
Affiliation:
Astrophysikalisches Institut Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany email: [email protected]
Ralf S. Klessen
Affiliation:
Insitut für Theoretische Astrophysik/Zentrum für Astronomie der Universität Heidelberg, Albert-Überle-Str. 2, D-69120, Germany email: [email protected]
Mordecai-Mark Mac Low
Affiliation:
Department of Astrophysics, American Museum of Natural History, 79th Street at Central Park West, New York, NY 10024-5192, USA email: [email protected]
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Abstract

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In cold dark matter cosmological models, the first stars to form are believed to do so within small protogalaxies. We study the influence of low levels of metal enrichment on the cooling and collapse of ionized gas in these protogalactic halos using three-dimensional, smoothed particle hydrodynamics simulations.

Keywords

stars: formationmethods: numericalhydrodynamicsearly Universe
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Highlights of Astronomy 14: Highlights of Astronomy , August 2006 , pp. 268
Copyright
Copyright © International Astronomical Union 2007

References

Kitsionas, S., & Whitworth, A. P. 2002, MNRAS, 330, 129Google Scholar
Jappsen, A.-K., Glover, S. C. O., Klessen, R. S., & Mac Low, M.-M. 2007, ApJ, 660, 1332Google Scholar