Cooling in Primordial Structure Formation

Details Cooling in Primordial Structure Formation Cooling in Primordial Structure Formation

Mar 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aipc..990...33m&link_type=abstract

FIRST STARS III: First Stars II Conference. AIP Conference Proceedings, Volume 990, pp. 33-35 (2008).

Physics

1

Origin, Formation, Evolution, Age, And Star Formation, Star Formation, Cosmology, Molecular Clouds, H2 Clouds, Dense Clouds, And Dark Clouds, Intracluster Matter, Cooling Flows, Dark Matter, Protogalaxies, Primordial Galaxies, Hydrodynamics

Scientific paper

Cooling is the main process leading to the condensation of gas in the dark matter potential wells. In a metal free environment, the main available coolants are H, He, H2 and HD molecules; once the gas is enriched with metals, their contribution becomes dominant. Here, we present our implementation, in the Gadget2 code, of molecular and metal line cooling at the temperatures (T<104 K) relevant for primordial structure formation.

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