Deuterium in the Universe

Details Deuterium in the Universe Deuterium in the Universe

Sep 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995apj...451...44p&link_type=abstract

Astrophysical Journal v.451, p.44

Astronomy and Astrophysics

Astronomy

45

Cosmology: Early Universe, Cosmology: Theory, Galaxies: Evolution, Nuclear Reactions, Nucleosynthesis, Abundances

Scientific paper

The role of deuterium is analyzed in the context of the chemical and thermal evolution of the gas component in the post-recombination universe. The formation of the main molecular species is followed as a function of the cosmological parameters Ω0, η, and H0. The abundance of H2 molecules is rather insensitive to the choice of the cosmological model, while less abundant species, such as HD and LiH, show large variations and can be used as potential diagnostics. The interaction of primordial molecules with the cosmic background radiation (CBR) is quite inefficient apart from LiH in the case of cosmological models with very small values of Ω0 and H0. In such cases, resonant scattering on the CBR photons can cause some partial blurring of primary anisotropies at a level that may be detected by ongoing experiments. Standard models of galactic evolution can easily reproduce the observed abundances of deuterium in the solar system and in the interstellar medium but fail badly to account for 3He. The discrepancy becomes even worse for models with high primordial D abundance (small values of η). We discuss several solutions that may be necessary if the high abundance of D recently measured toward high-redshift quasars is confirmed.

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