Energy conditions of the f(T, B) gravity dark energy model with the validity of thermodynamics

Abstract

In this article, the analysis of Tsallis holographic dark energy (which turns into holographic dark energy for a particular choice of positive non-additivity parameter δ) in modified f (T, B) gravity with the validity of thermodynamics and energy conditions for a homogeneous and isotropic FLRW Universe has been studied. The enlightenment of the field equation towards , made possible by the fact that the model is purely accelerating, corresponds to q = −0.54 (Mamon and Das 2017 Eur. Phys. J. C 77 49). The generalized second law of thermodynamics is valid not only for the same temperature inside the horizon, but also for the apparent horizon for a change in temperature. The essential inspiration driving this article is to exhibit the applicability that the holographic dark energy achieved from standard Tsallis holographic dark energy and the components acquired from f(T, B) gravity are identical for the specific bounty of constants. The analysis of energy conditions confirms that the weak energy condition and the null energy condition are fulfilled throughout the expansion, while violation of the strong energy condition validates the accelerated expansion of the Universe. With the expansion, the model becomes a quintessence dominated model. The dominant energy condition is not observed initially when the model is filled with genuine baryonic matter, whereas it appears when the model is in the quintessence dominated era.

Anisotropic behavior of universe in $$f(R, L_m)$$ gravity with varying deceleration parameter

“…9, 12, 13 and 14. These conditions have been rigorously examined and affirmed in diverse scenarios, such as the investigation of dark energy, dark matter, and cosmic expansion, with results consistent with prior studies [78][79][80][81][82].…”

Analysis of Reconstructed Modified Symmetric Teleparallel f(Q) Gravity

“…In the foregoing epoch, a lot of investigation has been primed in the modified theories of gravitation such as f(R), f(R, T ), f(G), f(R, G), and f(T, B) gravity, where R, G, T and T denotes the Ricci scalar, Gauss-Bonnet invariant, trace of energy-momentum tensor and torsion scalar of the Universe respectively. Innumeral works have been established in the framework of this modified theories of gravity and interesting results have been found in (Capozziello et al, 2007;Nojiri and Odintsov 2007;Azadi et al, 2008;Capozziello et al, 2008;Nojiri and Odintsov 2008;Harko et al, 2011;Daouda et al, 2012;Wei et al, 2012;Sharif and Yousaf 2013;Sahoo et al, 2014;Abbas et al, 2015;Chirde and Shekh 2015;Chirde and Shekh, 2016a;Chirde and Shekh, 2016b;Sharif and Fatima 2016;Bhatti et al, 2017;Bhoyar et al, 2017;Shekh, 2018a, Chirde andShekh, 2018b;Chirde and Shekh, 2019;Pawar et al, 2018;Shekh and Chirde, 2019;Shekh and Chirde, 2020;Shekh et al, 2020b;Dagwal and Pawar 2020;Sahoo and Bhattacharjee 2020;Shekh et al, 2020a;Shekh and Chirde 2020;Shekh et al, 2021;Shekh, 2021a;Shekh 2021b). Among the all determinations, one model which is based on the so-called f(Q) gravity theory or symmetric teleparallel gravity, where the nonmetricity scalar Q is works as gravitational interaction.…”

Observational constraints in accelerated emergent f(Q) gravity model

“…They discovered that the Gauss-Bonnet term's contribution to the linear and quadratic models behaves exactly like a cosmological constant, demonstrating the ΛCDM model, which is consistent with the observational findings and is similar to satellite experiments like the Wilkinson Microwave Anisotropic Probe. Recently, some alternative gravities are proposed as f(R, G) [36,37], f(T, B) gravity [38].…”