Quark stars in $$f(T, \mathcal {T})$$ f ( T , T ) -gravity

Pace, Mario; Said, Jackson Levi

doi:10.1140/epjc/s10052-017-4637-8

Cited by 62 publications

(38 citation statements)

References 34 publications

(56 reference statements)

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“…Also, in a further work, the analysis presented here can be performed in models of nonminimal torsion-matter coupling, like those in References [65,66]. While the hydrostatic equilibrium of quark stars has already been performed in such models [67], the application for neutron stars and WDs still lacks.…”

Section: Discussionmentioning

confidence: 99%

Stellar equilibrium configurations of white dwarfs in the f(R, T) gravity

Carvalho¹,

Lobato²,

Moraes³

et al. 2017

Eur. Phys. J. C

108

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In this work we investigate the equilibrium configurations of white dwarfs in a modified gravity theory, namely, f (R, T ) gravity, for which R and T stand for the Ricci scalar and trace of the energy-momentum tensor, respectively. Considering the functional form f (R, T ) = R +2λT , with λ being a constant, we obtain the hydrostatic equilibrium equation for the theory. Some physical properties of white dwarfs, such as: mass, radius, pressure and energy density, as well as their dependence on the parameter λ are derived. More massive and larger white dwarfs are found for negative values of λ when it decreases. The equilibrium configurations predict a maximum mass limit for white dwarfs slightly above the Chandrasekhar limit, with larger radii and lower central densities when compared to standard gravity outcomes. The most important effect of f (R, T ) theory for massive white dwarfs is the increase of the radius in comparison with GR and also f (R) results. By comparing our results with some observational data of massive white dwarfs we also find a lower limit for λ, namely, λ > −3 × 10 −4 .

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Section: Discussionmentioning

confidence: 99%

Stellar equilibrium configurations of white dwarfs in the f(R, T) gravity

Carvalho¹,

Lobato²,

Moraes³

et al. 2017

Eur. Phys. J. C

108

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“…In addition, some regular black hole solutions (perturbatively and exact) have been found correctly in [14,15]. When one considers matter, there are some works which have studied the possibility of constructing stars or wormhole solutions in different teleparallel theories of gravity [16][17][18][19][20][21][22][23][24]. Overall the issue of finding exact spherically symmetric solutions in f (T )-gravity is still an open problem.…”

Section: Introductionmentioning

confidence: 99%

Photon sphere and perihelion shift in weak f(T) gravity

2019

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Among modified theories of gravity, the teleparallel f (T ) gravity is an intensively discussed model in the literature. The best way to investigate its viability is to derive observable predictions which yield evidence or constraints for the model, when compared with actual observations. In this paper we derive the photon sphere and the perihelion shift for weak f (T ) perturbations of general relativity. We consistently calculate first order teleparallel perturbations of Schwarzschild and Minkowski spacetime geometry, with which we improve and extend existing results in the literature. * Electronic address: sbahamonde@ut.ee † Electronic address: kai.flathmann@uni-oldenburg.de ‡ Electronic address: christian.pfeifer@ut.ee

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“…Still, there are few exact spherically symmetric solutions in modified Teleparallel gravity. Different authors have studied stars and wormholes in different Teleparallel theories [27,[31][32][33][34]. In [20,35], the authors found some vacuum exact solutions in f (T ) gravity, however, they imposed T = constant, which is nothing but consider GR plus a cosmological constant.…”

Section: Introductionmentioning

confidence: 99%

Exact Spherically Symmetric Solutions in Modified Teleparallel Gravity

Bahamonde

Camcı²

2019

Symmetry

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Finding spherically symmetric exact solutions in modified gravity is usually a difficult task. In this paper we use the Noether's symmetry approach for a modified Teleparallel theory of gravity labelled as f (T, B) gravity where T is the scalar torsion and B the boundary term. Using the Noether's theorem, we were able to find exact spherically symmetric solutions for different forms of the function f (T, B) coming from the Noether's symmetries.

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Quark stars in $$f(T, \mathcal {T})$$ f ( T , T ) -gravity

Cited by 62 publications

References 34 publications

Stellar equilibrium configurations of white dwarfs in the f(R, T) gravity

Stellar equilibrium configurations of white dwarfs in the f(R, T) gravity

Photon sphere and perihelion shift in weak f(T) gravity

Exact Spherically Symmetric Solutions in Modified Teleparallel Gravity

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