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- W2174336833 abstract "A cosmological model is constructed which is a Friedmann model, but with a finite ultimate temperature (T F). The model predicts the temperature of the cosmic-microwave background in terms of 4 parameters: the present energy density of matter in the Universe and the parameters which may have characterized hot, dense, hadronic matter during the early Universe (A, T F, B). The latter are defined by the level density for hadronic matter: $$sigma (m)underrightarrow {m to infty } Am^{ - B} exp [m/T_F ]$$ . The calculation of the microwave temperature gives similar results for Hagedorn (B=5/2) and Frautschi (B=3) models. Both models clearly favour a low cosmic density ((10−31÷10−33) g/cm3) over a high density (10−29 g/cm3). This result suggests that hot, dense, hadronic matter in thermal contact with radiation in the early Universe conspired to produce the open Universe of today." @default.
- W2174336833 created "2016-06-24" @default.
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- W2174336833 date "1976-08-01" @default.
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- W2174336833 title "The role of strong interactions in cosmology" @default.
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- W2174336833 doi "https://doi.org/10.1007/bf02728605" @default.
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