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The thermal regime of the baryons behind shock waves arising in the process of virialization of dark matter halos is governed at certain conditions by radiation of HD lines. A small fraction of the shocked gas can cool down to the temperature of the cosmic microwave background (CMB). We estimate an upper limit for this fraction: at  z  = 10 it increases sharply from about  q T   ∼ 10 –3  for dark halos of  M  = 5 × 10 7  M ⊙  to ∼ 0.1 for halos with  M  = 10 8  M ⊙ . Further increase of the halo mass does not lead however to a significant growth of  q T   – the asymptotic value for  M  ≫ 10 8  M ⊙  is 0.3. We estimate the star formation rate associated with such shock waves, and show that they can provide a small but not negligible fraction of the star formation. We argue that extremely metal‐poor low‐mass stars in the Milky Way may have been formed from primordial gas behind such shocks. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)

Low‐temperature primordial gas in merging halos