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Remarks on the viscosity concept in the early universe. (English) Zbl 0820.76097

Summary: Some aspects of viscous cosmological models, mainly of Bianchi type-I, are studied, in particular with the purpose to obtain a natural explanation of why the entropy per baryon in the universe, \(\sigma\sim 10^ 9\), is so large. Using the FRW metric it is first shown that the expressions for the bulk viscosity as derived from kinetic theory in the plasma era are incapable of explaining the large value of \(\sigma\). However, it is possible to imagine the viscosity to be an “impulse” viscosity operative in one or several phase transitions in the early universe. This is the main idea elaborated on in the present paper. It is shown that in the \(k= 0\) FRW space, an impulse bulk viscosity \(\zeta_{\text{infl}}\sim 10^{60}\) g cm\(^{-1}s^{-1}\) acting at the phase transition at the end of the inflationary epoch corresponds to the correct entropy. If the space is anisotropic, it is natural to exploit the analogy with classical fluid dynamics to introduce the turbulent viscosity concept. This is finally discussed, in relation to an anisotropy introduced in the universe via the Kasner metric.

MSC:

76Y05 Quantum hydrodynamics and relativistic hydrodynamics
83F05 Relativistic cosmology
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