The Lithium Chemistry of the Early Universe

Details The Lithium Chemistry of the Early Universe The Lithium Chemistry of the Early Universe

Dec 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994aas...185.5501s&link_type=abstract

American Astronomical Society, 185th AAS Meeting, #55.01; Bulletin of the American Astronomical Society, Vol. 26, p.1405

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Calculations will be presented for the abundances of Li, Li(+) , LiH, and LiH(+) during the post recombination epoch of the early universe. Atomic lithium is found to remain significantly ionized with a fractional ionization f ~ 0.5 to redshifts z as small as 10. The abundance of LiH is determined to be ~ 10(2) smaller than obtained by previous calculations due to the inclusion of a new quantal radiative association rate coefficient. Inclusion of other gas-phase reactions further reduces the LiH abundance. LiH(+) is found to be less abundant than LiH. These low abundances suggest that Thomson scattering between cosmic background radiation (CBR) photons and primordial LiH and LiH(+) plays an insignificant role in erasing CBR anisotropies. Though the densities will increase in collapsing proto-clouds, the initially small abundances may severely limit searches for highly redshifted rovibrational lines and reduce their utility for constraining the cosmological Li abundance. The new LiH and LiH(+) radiative association rate coefficients will also be presented.

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