Bianchi type-III Tsallis holographic dark energy model in Saez–Ballester theory of gravitation

Abstract

In this paper, we have investigated Tsallis holographic dark energy (infrared cutoff is the Hubble radius) in homogeneous and anisotropic Bianchi type-III Universe within the framework of Saez–Ballester scalar–tensor theory of gravitation. We have constructed non-interaction and interaction dark energy models by solving the Saez–Ballester field equations. To solve the field equations, we assume a relationship between the metric potentials of the model. We developed the various cosmological parameters (namely deceleration parameter q, equation of state parameter $$\omega _t$$ ω t , squared sound speed $$v_s^2$$ v s 2 , om-diagnostic parameter Om(z) and scalar field $$\phi $$ ϕ ) and well-known cosmological planes (namely $$\omega _t-\omega _t^{'}$$ ω t - ω t ′ plane, where $$'$$ ′ denotes derivative with respect to ln(a) and statefinders ($$r-s$$ r - s ) plane) and analyzed their behavior through graphical representation for our both the models. It is also, quite interesting to mention here that the obtained results are coincide with the modern observational data.

Kantowski–Sachs Tsallis holographic dark energy model with sign-changeable interaction

“…Recently, Prasanthi and Aditya [66] have investigated BT-VI 0 Renyi HDE models in the frame-work of general relativity. Very recently, Santhi and Sobhanbabu [67,68] have studied BT-III and BT-VI 0 THDE models in Scalar tensor theories of gravitation.…”

Magnetized Bianchi Model with Time-dependent Deceleration Parameter

“…Further, the concept is also consistent with the flat ΛCDM model. In the Saez-Ballester modified theory of gravitation, Santhi and Sobhanbabu (4) also looked into the Tsallis holographic dark energy in Bianchi type III spacetime which coincides with the isotropic model discussed by Dixit et al (3) . In the discussion of the anisotropic Bianchi Type-III dark energy cosmological model with a massive scalar meson field in general relativity, Raju et al (5) noted that the EoS parameter of the model varies initially in the phantom region and then approaches the quintessence region as the model's physical parameters become independent of the scalar field at late times.…”

“…The result of the deceleration parameter follows the recent cosmological data. Some model also exhibits superexponential expansion at the early phase with q < −1 and, finally, at late times, tends to exponential expansion q = −1 (Santhi and Sobanbabu (4) ). • Initially, the dominant energy condition (DEC) gets violated for time t < 0.3, and then rapidly, it satisfies the energy condition as positively decreasing with time.…”

Barrow holographic dark energy models in f(Q) symmetric teleparallel gravity with Lambert function distribution

“…From the above continuity equation, we can see that the interaction term must be proportional to a quantity with units of inverse of cosmic time. Therefore, this term in the literature can take several forms (Qclasses) such as Q = 3ηHρ M , Q = 3ηHρ DE , and Q = 3ηH ρ M + ρ DE [53][54][55]. In this study, we choose Q = 3ηHρ B as an interaction term where 3ηH is the decay rate with a coupling constant η (interaction parameter) [56].…”