Abstract
The astrophysical importance of the Q-H phase transition comes from the fact that, below the critical temperature, it may induce in the cosmic fluid baryon density inhomogeneities, together with inhomogeneities in the ratio of neutrons to protons. These inhomogeneities could later modify the Big Bang nucleosynthesis yields of the four cosmological nuclides: D, 3He, 4He, 7Li, over the values obtained in the case of the Standard Big-Bang (homogeneous density).
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Reeves, H. (1990). Limits on the Cosmic Baryon Density. In: Vautherin, D., Lenz, F., Negele, J.W. (eds) Hadrons and Hadronic Matter. NATO ASI Series, vol 228. Springer, Boston, MA. https://doi.org/10.1007/978-1-4684-1336-6_11
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