Deuterium chemistry in the primordial gas

Abstract

We review and update some aspects of deuterium chemistry in the post-recombination Universe with particular emphasis on the formation and destruction of HD. We examine in detail the available theoretical and experimental data for the leading reactions of deuterium chemistry and we highlight the areas where improvements in the determination of rate coefficients are necessary to reduce the remaining uncertainties. We discuss the cooling properties of HD and the modifications to the standard cooling function introduced by the presence of the cosmological radiation field. Finally, we consider the effects of deuterium chemistry on the dynamical collapse of primordial clouds in a simple ``top-hat'' scenario, and we speculate on the minimum mass a cloud must have in order to be able to cool in a Hubble time.

22 pages, 10 figures, LaTeX. Earth and Planetary Sciences, in press

References in corpus (2)

• HD Molecular Lines in an Absorption System at Redshift z = 2.3377
• A new deuterium abundance measurement from a damped Ly-alpha system at z_abs = 3.025

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