Computer Science
Scientific paper
Mar 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aipc..990...30m&link_type=abstract
FIRST STARS III: First Stars II Conference. AIP Conference Proceedings, Volume 990, pp. 30-32 (2008).
Computer Science
Population Iii Stars, Cosmology, Star Formation, Molecular Clouds, H2 Clouds, Dense Clouds, And Dark Clouds, Hydrodynamics, Intracluster Matter, Cooling Flows, Atomic, Molecular, Chemical, And Grain Processes
Scientific paper
We describe results from 3D hydrodynamical simulations of primordial star formation including HD chemistry. In the first set of simulations we consider three star-forming halos at z~15 in ΛCDM cosmology, comparing runs with and without HD chemistry. HD has little influence on the formation of typical first generation stars, though we find evidence that in lower mass halos HD cooling can become effective. We also examined the effect of HD cooling in primordial ionized regions by flash-heating the same simulation volumes at z = 20 and repeating the runs. In ionized gas, HD is the dominant coolant for much of the collapsing cloud, lowering both the gas temperature and the expected stellar mass by a factor of 2-3 relative to runs without HD chemistry.
Bryan Greg L.
McGreer Ian D.
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