Curvature Inspired Cosmological Scenario

Abstract

Using modified gravity with non-linear terms of curvature, $R^2$ and $R^{(r+2)}$ (with $r$ being the positive real number and $R$ being the scalar curvature), cosmological scenario,beginning at the Planck scale, is obtained. Here, a unified picture of cosmology is obtained from $f(R)-$ gravity. In this scenario, universe begins with power-law inflation, followed by deceleration and acceleration in the late universe as well as possible collapse of the universe in future. It is different from $f(R)-$ dark energy models with non-linear curvature terms assumed as dark energy. Here, dark energy terms are induced by linear as well as non-linear terms of curvature in Friedmann equation being derived from modified gravity.It is also interesting to see that, in this model, dark radiation and dark matter terms emerge spontaneously from the gravitational sector. It is found that dark energy, obtained here, behaves as quintessence in the early universe and phantom in the late universe. Moreover, analogous to brane-tension in brane-gravity inspired Friedmann equation, a tension term $\lambda$ arises here being called as cosmic tension. It is found that, in the late universe, Friedmann equation (obtained here) contains a term $-{\rho }^2/2\lambda$ ($\rho$ being the phantom energy density) analogous to a similar term in Friedmann equation with loop quantum effects, if $\lambda >0$ and brane-gravity correction when $\lambda <0.$

19 Pages. To appear in Int. J. Thro. Phys

References in corpus (1)

• Conditions for the cosmological viability of f(R) dark energy models

Cited by in corpus (8)

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• Power-law cosmic expansion in f(R) gravity models
• On the co-existence of matter dominated and accelerating solutions in f(G)-gravity
• Dynamics of f(R)-cosmologies containing Einstein static models
• Dynamical systems analysis of anisotropic cosmologies in $R^n$-gravity
• Implications of non-analytical f(R) gravity at Solar-System scales
• Acceleration and Deceleration in Curvature Induced Phantom Model of the Late and Future Universe, Cosmic Collapse as Well as its Quantum Escape
• $f(R)$-Cosmolgy from Early Universe Upto Future Cosmic Collapse and its Avoidance