Abstract
Abstract
The acceleration of the Universe is described as a consequence of the extrinsic curvature of a four dimensional space–time embedded in a five dimensional bulk space, defined by the Einstein–Hilbert principle. Using the linear approximation of the Nash–Greene embedding theorem, we obtain the related perturbed equations in which only the gravitational-tensor field equations contribute to the propagation of the cosmological perturbations. In accordance with big bang nucleosynthesis and solar constraints, we calculate numerically the effective Newtonian function G
eff to constrain the related parameters of the model. We numerically solve the growth density equation for two possible family of solutions leading to growth overdensities and, in some cases, a mild damping of the growth profiles, with a top amplification of the growth perturbations around 14% in comparison with ΛCDM and wCDM models. The behaviour of the effective gravitational potential Φ and the Newtonian curvature Ψ is also analysed showing mild perturbations in early times induced only by the extrinsic curvature differently from the ΛCDM standards.
Funder
Fundação Araucária
Federal University of Latin America integration
Subject
Physics and Astronomy (miscellaneous)
Cited by
1 articles.
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