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Numerical solutions to the cosmological 3-fluid problem

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Abstract

We show that, for the scalar field cosmology with exponential potential, the set of values of the coupling parameter for which the solutions undergo a transient period of acceleration (TPA) is much larger than the set discussed in the literature. The gradual inclusion of ordinary and dark matters results in an everywhere, but near the origin, smoother and right shifted (along the time axis) acceleration curve. For the 3-fluid problem, the energy density need not exhibit a plateau during the acceleration period. Much excess in the dark matter and/or ordinary matter energy densities would lead the universe to undergo an eternal deceleration expansion. For the 3-fluid problem with a single exponential potential we conclude that the Big Bang Nucleosynthesis constraint is not fulfilled if the universe is to undergo a TPA. The 3-fluid model remains a good approximation for the description of large scale structures.

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Notes

  1. The second term in Eq. (20) of Ref. [20] should read \(-\varepsilon ka^3\dot{\phi }^2/2\).

  2. Because of different conventions, the values of (\(\lambda _R,V_{0R}\)) used in [8] are such that \(\lambda =\sqrt{6}\lambda _R\) and \(V_{0R}=6V_0\).

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  1. Department of Mathematics, Başkent University, Bağlıca Campus, Ankara, Turkey

    Mustapha Azreg-Aïnou

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Correspondence to Mustapha Azreg-Aïnou.

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Azreg-Aïnou, M. Numerical solutions to the cosmological 3-fluid problem. Gen Relativ Gravit 45, 2635–2646 (2013). https://doi.org/10.1007/s10714-013-1607-9

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