Abstract
Most relevant observations agree with the standard “big bang” model in which the universe started to expand about 1.6E10 yrs. ago from a state of high density and high temperature. 1H and 4He and (in very minor quantities) their isotopes 2H = D and 3He formed at an expansion time t ~ 300 s. However, no elements with atomic number A ≥ 4 could form by neutron capture, the process by which D through 4He formed. In Table 1 I have compiled what I consider to be the best estimates of the primordial abundances (see also Section 2.5 and Wagoner, 1973). At t ~ 3E5 yrs. and temperatures of ~3000 K, free electrons combined with protons and He-nuclei and the radiation field decoupled from the matter. Today the radiation field is observed as an isotropic black-body background radiation of radiation temperature 2.7 K (see Fig. 5). Density fluctuations present in the primordial matter increased as a result of the expansion of the universe and protogalactic clouds formed with masses ranging from 1E12 MO to lE8 MO (and possibly less).
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Mezger, P.G. (1978). Interstellar Matter. In: Setti, G., Fazio, G.G. (eds) Infrared Astronomy. NATO Advanced Study Institutes Series, vol 38. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-9815-5_1
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