Reconstructing f(T) modified gravity from ECHDE and ECNADE models

We investigate alternative candidates to dark energy (DE) that can explain the current state of the Universe in the framework of the generalized teleparallel theory of gravity f(T), where T denotes the torsion scalar. To achieve this, we carry out a series of reconstructions taking into account the ordinary and entropy-corrected versions of the holographic and new agegraphic DE models. These models are used as alternatives to DE in the literature in order to describe the current state of our Universe. It is remarked that the proposed models indicate behavior akin to phantom or quintessence models. Furthermore, we also generate the parameters of the equation of state associated with entropy-corrected models and we observe a phase transition between the quintessence state and phantom state as it is shown by the recent observational data. We also investigate the stability of these models and we create the $\{r-s\}$ trajectories and compare with the ΛCDM limit. The behavior of certain physical parameters such as the speed of sound and the Statefinder diagnostic pair $\{r-s\}$ is compatible with the current observational data.     

Slow-roll inflation in non-geometric flux compactification

By implementing a genetic algorithm we search for stable vacua in Type IIB non-geometric flux compactification on an isotropic torus with orientifold 3-planes. We find that the number of stable dS and AdS vacua are of the same order. Moreover we find that in all dS vacua the multi-field slow-roll inflationary conditions are fulfilled. Specifically we observe that inflation is driven by the axio-dilaton and the Kähler moduli. We also comment on the existence of one stable dS vacuum in the presence of exotic orientifolds.     

Tensor perturbations from bounce inflation scenario in f(Q) gravity

In this paper, we construct a bounce inflation cosmological scenario in the framework of the modified symmetric teleparallel gravity, namely f(Q) theory, and investigate the tensor perturbations therein. As is well-known, the tensor perturbations generated in the very early Universe(inflation and pre-inflation regions) can account for the primordial gravitational waves(PGWs) that are to be detected by the next generation of GW experiments. We discuss the stability condition of the tensor perturb...     

Thin-shell gravastar model in f(Q,T) gravity

In the last few decades,gravastars have been proposed as an alternative to black holes.The stability of a gravastar has been examined in many modified theories of gravity along with Einstein s GR.The f(Q,T) gravity,a successfully modified theory of gravity for describing the current accelerated expansion of the universe,has been used in this study to examine gravastar in different aspects.According to Mazur and Mottola [Proc.Natl.Acad.Sci.101,9545(2004);Gravitational condensate stars:An alternat...     

Bianchi type-I cosmology in f(R,T) gravity

We investigate the exact solutions of a Bianchi type-I space-time in the context of f(R, T) gravity [1], where f(R, T) is an arbitrary function of the Ricci scalar R and the trace of the energy-momentum tensor T. For this purpose, we find two exact solutions using the assumption of a constant deceleration parameter and the variation law of the Hubble parameter. The obtained solutions correspond to two different models of the Universe. The physical behavior of these models is also discussed.     

Charged quark stars in f(R,T) gravity

Recent advances in nuclear theory and new astrophysical observations have led to the need for specific theoretical models applicable to dense-matter physics phenomena. Quantum chromodynamics (QCD) predicts the existence of non-nucleonic degrees of freedom at high densities in neutron-star matter, such as quark matter. Within a confining quark matter model, which consists of homogeneous, neutral 3-flavor interacting quark matter with \begin{document}$ \mathcal{O}(m_s^4) $\end{document} corrections, we examine the structure of compact stars composed of a charged perfect fluid in the context of \begin{document}$ f(R,T) $\end{document} gravity. The system of differential equations describing the structure of charged compact stars has been derived and numerically solved for a gravity model with \begin{document}$ f(R,T)= R+ 2\beta T $\end{document}. For simplicity, we assumed that the charge density is proportional to the energy density, namely, \begin{document}$ \rho_{\rm ch} = \alpha \rho $\end{document}. It is demonstrated that the matter-geometry coupling constant β and charge parameter α affect the total gravitational mass and the radius of the star.     

Geodesic deviation equation in f(R,T) gravity

In this paper, we investigate the modified Geodesic Deviation Equation (GDE) in the framework of f(R, T) theory of gravity where R and T are the curvature scalar and the trace of the energy-momentum tensor, respectively, using the FLRW background. In this way, we obtain the GR equivalent (GDE) in f(R, T) metric formalism. We also extend our work to the generalization of the Matting relation and perform the numerical analysis with GDE for null vector.     

Dynamical wormhole solutions in f(T) gravity

We study dynamical wormhole solutions in the framework of $f(T)$ f ( T ) theory of gravity with anisotropic fluid. We assume a general dynamical spherically symmetric wormhole spacetime with specific form of the shape function and scale factor. The scale factor is taken in the power-law form in order to meet the accelerated expansion of the universe. We discuss the behavior of energy conditions for three particular choices of equation of state, i.e., radial and transverse pressures in linear form with energy density and traceless fluid. The energy conditions satisfy for certain time intervals in all cases. The radial coordinate does not play any role in graphs and the validity or violation of energy conditions depend upon the time coordinate only. The graphical behavior of the energy conditions become equivalent for radial and transverse pressures in all the three cases.     

Pilgrim dark energy in f(T) gravity

We discuss the interacting f(T) gravity with pressureless matter in an FRW spacetime. We construct an f(T) model by following the correspondence scheme incorporating a recently developed pilgrim dark energy model and taking the Hubble horizon as the IR cutoff. We use constructed model to discuss the evolution trajectories of the equation-of-state parameter, the ω _T -ω′ _T phase plane, and state-finder parameters in the evolving universe. It is found that the equation-of-state parameter gives a phantom era of the accelerated universe for some particular range of the pilgrim parameter. The ω _T -ω′ _T plane represents freezing regions only for an interacting framework, while the ΛCDM limit is attained in the state-finder plane. We also investigate the first and second laws of thermodynamics assuming equal temperatures at and inside the horizon in this scenario. Due to the violation of the first law of thermodynamics in f(T) gravity, we explore the behavior of the entropy production term. The validity of a generalized second law of thermodynamics depends on the present-day value of the Hubble parameter.     

Swampland dS conjecture in mimetic f(R,T) gravity

In this paper, we study a theory of gravity called mimetic f(R, T) in the presence of swampland dS conjecture. For this purpose, we introduce several inflation solutions of the Hubble parameter H(N) from f(R, T) = R + δT gravity model, in which R is Ricci scalar, and T denotes the trace of the energy–momentum tensor. Also, δ and N are the free parameter and a number of e-fold, respectively. Then we calculate quantities such as potential, Lagrange multiplier, slow-roll, and some cosmological parameters such as n_s and r. Then we challenge the mentioned inflationary model from the swampland dS conjecture. We discuss the stability of the model and investigate the compatibility or incompatibility of this inflationary scenario with the latest Planck observable data.     

Vacuum spherically symmetric solutions in f(T) gravity

Spherically symmetric static vacuum solutions have been built in f(T) models of gravity theory. We apply some conditions on the metric components; then new vacuum spherically symmetric solutions are obtained. Also, by extracting metric coefficients we determine the analytical form of f(T).