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Reconstructed f(R) Gravity and Its Csmological Consequences in Chameleon Scalar Field with A Scale Factor Describing The Pre-Bounce Ekpyrotic Contraction
Karmakar, S.; Myrzakulov, K.; Chattopadhyay, S.; Myrzakulov, R. Reconstructed f(R) Gravity and Its Cosmological Consequences in theChameleon Scalar Field with a Scale Factor Describing the Pre-Bounce Ekpyrotic Contraction. Symmetry2020, 12, 1559.
Karmakar, S.; Myrzakulov, K.; Chattopadhyay, S.; Myrzakulov, R. Reconstructed f(R) Gravity and Its Cosmological Consequences in theChameleon Scalar Field with a Scale Factor Describing the Pre-Bounce Ekpyrotic Contraction. Symmetry 2020, 12, 1559.
Karmakar, S.; Myrzakulov, K.; Chattopadhyay, S.; Myrzakulov, R. Reconstructed f(R) Gravity and Its Cosmological Consequences in theChameleon Scalar Field with a Scale Factor Describing the Pre-Bounce Ekpyrotic Contraction. Symmetry2020, 12, 1559.
Karmakar, S.; Myrzakulov, K.; Chattopadhyay, S.; Myrzakulov, R. Reconstructed f(R) Gravity and Its Cosmological Consequences in theChameleon Scalar Field with a Scale Factor Describing the Pre-Bounce Ekpyrotic Contraction. Symmetry 2020, 12, 1559.
Abstract
Inspired by the work of S. D. Odintsov and V. K. Oikonomou, Phys. Rev. D92, 024016 (2015) [1], the present study reports a reconstruction scheme for f (R) gravity with the scale factor a(t) µ (t * - t) c22describing the pre-bounce ekpyrotic contraction, where t is the big crunch time. The reconstructed f (R) is used to derive expressions for density and pressure contributions and the equation of state parameter resulting from this reconstruction is found to behave like "quintom". It has also been observed that the reconstructed f (R) has satisfied a sufficient condition for a realistic model. In the subsequent phase the reconstructed f (R) is applied to the model of chameleon scalar field and the scalar field f and the potential V(f) are tested for quasi-exponential ex pansion. It has been observed that although the reconstructed f (R) satisfies one of the sufficient conditions for realistic model, the quasi-exponential expansion is not available due to this reconstruction. Finally, the consequences pre-bounce ekpyrotic inflation i n f (R) gravity are compared to the background solution for f (R) matter bounce.
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