Open AccessThe cooling of shock‐compressed primordial gas
Author(s) -
Johnson Jarrett L.,
Bromm Volker
Publication year - 2006
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1111/j.1365-2966.2005.09846.x
Subject(s) - physics , astrophysics , cosmic microwave background , redshift , radiative cooling , stars , dark matter , astronomy , galaxy , quantum mechanics , anisotropy
We find that at redshifts z ≳ 10, HD line cooling allows strongly shocked primordial gas to cool to the temperature of the cosmic microwave background (CMB). This temperature is the minimum value attainable via radiative cooling. Provided that the abundance of HD, normalized to the total number density, exceeds a critical level of ∼10 −8 , the CMB temperature floor is reached in a time which is short in comparison to the Hubble time. We estimate the characteristic masses of stars formed out of shocked primordial gas in the wake of the first supernovae, and resulting from the virialization of dark matter haloes during hierarchical structure formation to be ∼10 M ⊙ . In addition, we show that cooling by HD enables the primordial gas in relic H ii regions to cool to temperatures considerably lower than those reached via H 2 cooling alone. We confirm that HD cooling is unimportant in cases where the primordial gas does not go through an ionized phase, as in the formation process of the very first stars in z ≳ 20 minihaloes of mass ∼10 6 M ⊙ .