Physical Acceptability of the Renyi, Tsallis and Sharma-Mittal Holographic Dark Energy Models in the f(T,B) Gravity under Hubble’s Cutoff

Salim Harun Shekh,Pradyumn Kumar Sahoo,Pedro H R S Moraes

doi:10.3390/universe7030067

Abstract

In the present article, we investigate the physical acceptability of the spatially homogeneous and isotropic Friedmann–Lemâitre–Robertson–Walker line element filled with two fluids, with the first being pressureless matter and the second being different types of holographic dark energy. This geometric and material content is considered within the gravitational field equations of the f(T,B) (where T is the torsion scalar and the B is the boundary term) gravity in Hubble’s cut-off. The cosmological parameters, such as the Equation of State (EoS) parameter, during the cosmic evolution, are calculated. The models are stable throughout the universe expansion. The region in which the model is presented is dependent on the real parameter δ of holographic dark energies. For all δ≥4.5, the models vary from ΛCDM era to the quintessence era.

Highlights

The amazing disclosure of the increasing expansion of the universe is one of the energizing advancement areas of cosmology
Energized by the above references, in this article, we investigate the Renyi, Tsallis and Sharma–Mittal holographic dark energy (HDE) models in the f (T, B) gravity under Hubble’s cutoff
The holographic principles need the degrees of freedom of a spatial region to reside not in the interior of an ordinary quantum field theory, but on the surface of the region, along with a number of degrees of freedom per unit area no greater than 1 per Planck area

Summary

Introduction

The amazing disclosure of the increasing expansion of the universe is one of the energizing advancement areas of cosmology. In [17], the first HDE model was proposed, where the holographic principle applies to cosmic acceleration Such a model of dark energy density relies on two physical quantities on the universe’s boundary: the reduced Planck mass and a cosmological length scale (which can be taken as the future event horizon of the universe).

H4 8πd d πδ H2 δ

Discussion