We investigate in this paper the structures of neutron stars under the strong magnetic field in the framework of f (T ) gravity where T denotes the scalar torsion. The TOV equations in this theory of gravity have been considered and numerical resolution of these equations has been performed within perturbative approach taking into account the equation of state of neutron dense matter in magnetic field. We simplify the problem by considering the very strong magnetic field which affects considerably the dense matter; and for quadratic and cubic corrections to Teleparallel term, one finds that the mass of neutron stars can increase for different values of the perturbation parameter. The deviation from Teleparallel for different values of magnetic field is found out and this feature is very appreciable in the case of cubic correction. Our results are related to the hadronic particles description with very small hyperon contributions and the mass-radius evolution is consistency with the observational data.
In this paper we explore f (T, T ), where T and T denote the torsion scalar and the trace of the energy-momentum tensor respectively. We impose the covariant conservation to the energymomentum tensor and obtain a cosmological f (T, T ) respectively. We impose the covariant conservation to the energy-momentum tensor and obtain a cosmological f (T, T ) model. Then, we study the stability of the obtained model for power-law and de Sitter solutions and our result show that the model can be stable for some values of the input parameters, for both power-law and de Sitter solutions.
We investigate in this paper the Landau–Lifshitz energy distribution in the framework of [Formula: see text] theory view as a modified version of Teleparallel theory. From some important Teleparallel theory results on the localization of energy, our investigations generalize the Landau–Lifshitz prescription from the computation of the energy–momentum complex to the framework of [Formula: see text] gravity as it is done in the modified versions of General Relativity. We compute the energy density in the first step for three plane-symmetric metrics in vacuum. We find for the second metric that the energy density vanishes independently of [Formula: see text] models. We find that the Teleparallel Landau–Lifshitz energy–momentum complex formulations for these metrics are different from those obtained in General Relativity for the same metrics. Second, the calculations are performed for the cosmic string spacetime metric. It results that the energy distribution depends on the mass [Formula: see text] and the radius [Formula: see text] of cosmic string and it is strongly affected by the parameter of the considered quadratic and cubic [Formula: see text] models. Our investigation with this metric induces interesting results susceptible to be tested with some astrophysics hypothesis.
Cosmological approaches of autonomous dynamical system in the framework of f (T ) gravity are investigated in this paper. Our methods applied to flat Friedmann-Robertson-Walker equations in f (T ) gravity, consist to extract dynamical systems whose time-dependence is contained in a single parameter m depending on the Hubble rate of Universe and its second derivative. In our attempt to investigate the autonomous aspect of the dynamical systems reconstructed in both vacuum and nonvacuum f (T ) gravities, two values of the parameter m have been considered for our present analysis. In the so-called quasi-de Sitter inflationary era (m ≃ 0), the corresponding autonomous dynamical systems provide stable de Sitter attractors and unstable de Sitter fixed points. Especially in the vacuum f (T ) gravity, the approximate form of the f (T ) gravity near the stable and the unstable de Sitter fixed points has been performed. The matter dominated era case (m = − 9 2 ) leads to unstable fixed points confirming matter dominated era or not, and stable attractor fixed point describing dark energy dominated era. Another subtlety around the stable fixed point obtained at matter dominated case in the non-vacuum f (T ) gravity is when the dark energy dominated era is reached, at the same time, the radiation perfect fluid dominated succumbs.
The geodesic deviation equation has been investigated in the framework of f (T, T ) gravity, where T denotes the torsion and T is the trace of the energy-momentum tensor, respectively. The FRW metric is assumed and the geodesic deviation equation has been established following the General Relativity approach in the first hand and secondly, by a direct method using the modified Friedmann equations. Via fundamental observers and null vector fields with FRW background, we have generalized the Raychaudhuri equation and the Mattig relation in f (T, T ) gravity. Furthermore, we have numerically solved the geodesic deviation equation for null vector fields by considering a particular form of f (T, T ) which induces interesting results susceptible to be tested with observational data.
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