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Since the scale factor is related to the energy density as ρ∼a−3(1+ωeff), where ωeff is the effective equation of state during the reheating, we have Nrh=ln(arhae)=−13(1+ωeff)ln(ρrhρe). (25) Now, we use the relation between the wave number and the ...
2 The figure describes the value of the matter density parameter m as a function of dark matter equation of state parameter wm and the strength of the potential energy, encoded into the value of the λ coefficient From the above expressions we can note that this solu- tion has a high ...
In fact, we consider the Gauss–Bonnet coupling as not having any contribution to the energy density due to this new parameter and the standard slow-roll parameters become | i | 1 and |δi | 1. During inflation we consider the slow-roll approximation where φ˙2 1 and φ¨ 3H φ˙....