Thermodynamical aspects of Bianchi type-I Universe in quadratic form of $f\left( Q\right) $ gravity and observational constraints

Abstract

In this paper, we study a LRS Bianchi type-I cosmological model in the framework of symmetric teleparallel f (Q) gravity in which the non-metricity term (Q) is responsible for the gravitational interaction. We have considered a special form of the f (Q) gravity function which can be cast as f (Q) = γ Q n (where γ and n are both the dynamical model constant parameters). Such a choice can be viewed as a hybrid scale factor and the cosmic time and the redshift are related viawhich describes a ΛCDM model of the Universe with the expansion evolving from decelerating to an acceleration phase. We further study the validity of our model with an investigation of the thermodynamical quantities and energy conditions along with some physical variables such as the EoS, jerk, and statefinder parameters. Our results are discussed in the light of current observational data and trends.

Bulk viscous fluid in extended symmetric teleparallel gravity

“…Cosmological solutions and growth index of matter perturbations have been evaluated for a polynomial functional form of f (Q) gravity in [18]. Assuming the power-law function, the coupling of matter in f (Q) gravity analyzed by Harko et al in [22] along with many other works mentioned in [23][24][25][26][27].…”

Anisotropic solutions in symmetric teleparallel $$f\left( Q\right) $$-theory: Kantowski–Sachs and Bianchi III LRS cosmologies

“…Some previous studies in the literature on anisotropic spacetimes in symmetric teleparallel f (Q)-theory are presented in [64][65][66][67]. In [68][69][70] the anisotropic Bianchi type I spacetime in the coincidence gauge in f (Q)-gravity was investigated, while the isotropic limit in such a cosmology was studied in [71]. The Bianchi type I geometry in the isotropic limit reduces to the spatially flat FLRW geometry.…”

Anisotropic f(Q) gravity model with bulk viscosity

“…In this work, we will examine a cosmological model in order to explain the cosmic acceleration in the framework of f (Q) symmetric teleparallel gravity proposed by Jiménez et al [23], where the non-metricity scalar Q is responsible for the gravitational interaction in this theory. Energy conditions [24], cosmography [25], spherically symmetric configuration [26], signature of f (Q) gravity [27], growth index of matter perturbations [28], coupling matter [29], quantum cosmology for a f (Q) polynomial model [30], geodesic deviation equation [31], isotropization of LRS Bianchi-I Universe [32], etc, all these topics have been discussed in the framework of f (Q) gravity by several researchers and also the reader can see our work in this context [33][34][35][36][37].…”

“…The physical justification for this presumption is imposed on the basis of the observations of the velocity redshift relation for extragalactic sources which propose that the Hubble expansion of the Universe may achieve isotropy when σ θ is constant [48]. This condition has been used in many works [32,36,37]. Using Eq.…”