Strong magnetic field effects on neutron stars within f(T) theory of gravity

Ganiou, M. G.; Ainamon, Cyrille; Houndjo, M. J. S.; Tossa, J.

doi:10.1140/epjp/i2017-11499-3

Cited by 18 publications

(12 citation statements)

References 58 publications

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“…In fact, there are papers in the literature related to compact stars in f (T ) gravity [9][10][11]24] in which very complicated equations are obtained for different tetrads, as well as for some ansatz for B and or T , for example.…”

Section: Compact Stars On F (T ) Modelsmentioning

confidence: 99%

“…With this specific choice for f (T ), taking γ = −π/2 1 in order to get rid of the restriction on f (T ) from ( 8) and by considering the hydrostatic equilibrium ( Ḃ = 0, Ȧ = 0), equations (7)(8)(9)(10)(11) can be rewritten as:…”

Section: Compact Stars On F (T ) Modelsmentioning

confidence: 99%

“…For this, it is necessary to obtain the TOV equations corresponding to the model in question and look for solutions of these equations. The proposal is to obtain these solutions for neutron stars from a more general approach than those already presented in the literature [9][10][11].…”

Section: Introductionmentioning

confidence: 99%

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Solving Tolman-Oppenheimer-Volkoff equations in $f(T)$ gravity: a novel approach

Fortes,

de Araujo

2021

Preprint

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The torsion models have stood out among the proposals for an alternative description of gravity. The simplest of them, the Teleparallel theory, is equivalent to General Relativity and there are many studies that seek to study its extension to more general functions of the torsion T . The purpose of our study is to consider a family of f (T ) models and apply their corresponding Tolman-Oppenheimer-Volkof equations to compact objects such as neutron stars. Consequently, through a numerical analysis, calculate, among other things, the maximum mass allowed by the model for a neutron star, which would also allow us to evaluate which models are in accordance with observations. In the present paper, the first in the series, we show explicitly the set of equations that must be solved, and how to solve it, in order to model compact stars in f (T ) gravity without the need to adopt any particular form for the metric functions or consider any perturbative approach, as has been done in some works in the literature.

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Section: Compact Stars On F (T ) Modelsmentioning

confidence: 99%

Section: Compact Stars On F (T ) Modelsmentioning

confidence: 99%

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Solving Tolman-Oppenheimer-Volkoff equations in $f(T)$ gravity: a novel approach

Fortes,

de Araujo

2021

Preprint

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“…Then, one obtains nontrivial coupled differential equations which mix all the functions and their derivatives, namely as B, B , A and A . In general, we find in the literature this type of equations being solved by considering some approximations, restriction of the functions or perturbative calculations [17]- [19] in order to avoid a cumbersome process.…”

Section: Introductionmentioning

confidence: 99%

Solving Tolman-Oppenheimer-Volkoff equations in $f(T)$ gravity: a novel approach applied to polytropic equations of state

Araújo¹,

Fortes²

2021

Preprint

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The Teleparallel Theory is an alternative theory of gravity equivalent to General Relativity (GR) and with non-vanishing torsion T . Some extensions of this theory, the so-called f (T ) models, have been subject of many recent works. The purpose of our work in the end is to consider recent results for a specific family of f (T ) models by using their corresponding Tolman-Oppenheimer-Volkof to describe compact objects such as neutron stars. By performing numerical calculations, it is possible to find, among other things, the maximum mass allowed by the model for a neutron star for a given equation of state (EOS), which would also allow us to evaluate which models are in accordance with observations. To begin with, the present work, the second in the series, considers polytropic EOSs since they can offer a simpler and satisfactory description for the compact objects. In addition, with these EOSs, we can already assess how different the f (T ) theories are in relation to GR with respect to the stellar structure. The results already known to GR must be reproduced to some extent and, eventually, we can find models that allow higher maximum masses than Relativity itself, which could explain, for example, the secondary component of the event GW190814. This particular issue will be subject of a forthcoming paper, the third in the series, where realistic EOSs are considered.

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“…However, some astrophysical applications of f (T) gravity can be observed in the following works [53,54,55,56,57,59,60,61,62,63,64,65,66,67,68,69,70,71,72,73,74]. Böhmer et al [53] examined the existence of relativistic stars in f (T) gravity and explicitly constructed several classes of static perfect fluid solutions as well as the conservation equation for two different choices of tetrad.…”

Section: Introductionmentioning

confidence: 99%

Study of gravastars under $f(\mathbb{T})$ gravity

Das,

Ghosh,

Deb

et al. 2020

Preprint

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In the present paper we propose a stellar model under the f (T) gravity following the conjecture of Mazur-Mottola [Report number: LA-UR-01-5067 (2001); Proc. Natl. Acad. Sci. USA 101 ( 2004) 9545] known in literature as gravastar, a viable alternative to the black hole. This gravastar has three different regions, viz., (A) Interior core region, (B) Intermediate thin shell, and (C) Exterior spherical region. It is assumed that in the interior region the fluid pressure is equal to a negative matter-energy density providing a constant repulsive force over the spherical thin shell. This shell at the intermediate region is assumed to be formed by a fluid of ultrarelativistic plasma and the pressure, which is directly proportional to the matter-energy density according to Zel'dovich's conjecture of stiff fluid [Zeldovich, Mon. Not. R. Astron. Soc. 160 (1972) 1], does nullify the repulsive force exerted by the interior core region for a stable configuration. On the other hand, the exterior spherical region can be described by the exterior Schwarzschild-de Sitter solution. With all these specifications we have found out a set of exact and singularity-free solutions of the gravastar which presents several physically interesting as well as valid features within the framework of alternative gravity.

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Strong magnetic field effects on neutron stars within f(T) theory of gravity

Cited by 18 publications

References 58 publications

Solving Tolman-Oppenheimer-Volkoff equations in $f(T)$ gravity: a novel approach

Solving Tolman-Oppenheimer-Volkoff equations in $f(T)$ gravity: a novel approach

Solving Tolman-Oppenheimer-Volkoff equations in $f(T)$ gravity: a novel approach applied to polytropic equations of state

Study of gravastars under $f(\mathbb{T})$ gravity

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