Abstract
A spherically symmetric wormhole family of solutions, with null red-shift, in the context of f(R)-gravity is presented. The model depends on two parameters: m and beta and meets all requirements to be an asymptotically and traversable wormhole. To solve the field equations, an EoS is imposed: p_{perp }=-rho . It is found that for m=1 the solution satisfies the null energy condition, although F(R)<0 everywhere. For m=0, the model satisfies the null energy condition away from the throat, where the function F(R) is everywhere positive and together with dF(R)/dR vanish at the throat of the wormhole. This fact is beyond the scope of the non-existence theorem. Furthermore, the cosmological viability of the model, to address the late – time accelerated epoch, is analyzed on the background of a flat FLRW space-time. The model satisfies consistency of local gravity tests, stability under cosmological perturbations, ghosts free and stability of the de Sitter point.
Highlights
Its consequence is the presence of high derivative terms, which could in principle explain the accelerated expansion and the existence of dark energy or dark matter without the addition of extra matter fields
In order to achieve it we propose a new ansatz for the shape function b(r ) depending on two parameters m and β, and impose an equation of state relating the components of the energy–momentum tensor threading the throat of the wormhole, ρ⊥ = −ρ
To check the feasibility of our model, we have explored the cosmological properties of the obtained f (R) models to address the latetime cosmic acceleration of the Universe
Summary
Modified gravity theories such as f (R) and f (R, T ) gravity are promised scenarios to investigate wormhole regions satisfying energy conditions. To check the feasibility of our model, we have explored the cosmological properties of the obtained f (R) models to address the latetime cosmic acceleration of the Universe (issue related with the dark energy problem) In this regard, the resulting f (R) Lagrangian satisfies the general requirements to face this point [77], such as: (i) ghost free consistency, (ii) consistency with local gravity and stability under cosmological perturbations, (iii) stability at late-time de Sitter point. 6 some cosmological properties related with the accelerated expansion at late time of the Universe (dark energy) are discussed, and the Hubble rate and scale factor satisfying the field equations in the flat FLRW regime with an isotropic fluid are shown.
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