RHDE models in FRW Universe with two IR cut-offs with redshift parametrization
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RHDE models in FRW Universe with two IR cut-offs with redshift parametrization Archana Dixita , Vinod Kumar Bhardwajb , Anirudh Pradhanc Department of Mathematics, Institute of Applied Sciences and Humanities, GLA University, Mathura, Uttar Pradesh 281 406, India Received: 11 August 2020 / Accepted: 9 October 2020 © Società Italiana di Fisica and Springer-Verlag GmbH Germany, part of Springer Nature 2020
Abstract In this manuscript, we have researched the cosmic expansion phenomenon in flat FRW Universe through the interaction of the recently proposed Rènyi holographic dark energy (RHDE). For this reason, we assumed Hubble (H) and Granda–Oliveros (GO) horizons as IR cut-off in the framework of f (R, T ) gravity. With this choice for IR cut-off, we can obtain some important cosmological quantities such as the equation of state ωT , energy density ρT , density parameter T , and pressure pT , which are the function of the redshift z. It is observed that in both IR cut-offs the EoS parameter displays quintom-like behaviour for three different values of δ. Here, we plot these parameters versus redshift z and discuss the consistency of the recent findings. Next, we explore the ωT –ωT plane and the stability analysis of the dark energy model by a perturbation method. Our findings demonstrate that the Universe is an accelerating model of rapid growth that is explained by quintom like behaviour. Hence, the feasibility of the RHDE model with Hubble and GO cut-off is supported by our model. The results indicate that the IR cut-offs play a significant role in the understanding of the dynamics of the universe.
1 Introduction Observational information received by (SNIa) [1,2], large scale structures (LSS) [3–5] and cosmic microwave background (CMB), anisotropies [6,7] confirmed the present accelerated expansion of the universe. The dark energy is assumed as a responsible candidate for this present scenario of accelerated Universe [8–10]. The character of DE is unknown, and mysterious. The easiest choice for DE is cosmological constant with positive energy density and negative pressure. The cosmological constant faces several challenges, such as the issue of fine tuning, and the problem of coincidence [8]. One reasonable way of relieving the question of cosmic coincidence is to assume that dark matter (DM) and dark energy (DE) interact. For the complex DE scenario, there are different alternate theories suggested by observing the accelerating universe: (a) the scalar-field models of DE including quintessence [11], tachyon [12], k-
a e-mail: [email protected] b e-mail: [email protected] c e-mail: [email protected] (corresponding author)
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essence [13], (b) the interacting DE models including chaplygin gas [14], polytropic gas [15,16], phantom [17] and holographic dark energy (HDE) [18,19]. On the other hand, the nature of DE can be investigated on the basis of certain principles of quantum gravity, which would be the yiel
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