Anisotropic strange quintessence stars in f(T) gravity

Abbas, G.; Qaisar, Shahid; Meraj, M. A.

doi:10.1007/s10509-015-2389-1

Cited by 31 publications

(30 citation statements)

References 41 publications

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“…In the literature this feature is wrongly interpreted as "the diagonal tetrad is not a good tetrad for spherically-symmetric solutions in f (T ) gravity" [65][66][67][68][69][70][71][72][73][74][75][76][77][78][79][80][81].…”

Section: Spherically Symmetric Geometrymentioning

confidence: 99%

The covariant formulation of f ( T ) gravity

Krššák

Saridakis

2016

Class. Quantum Grav.

315

251

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We show that the well-known problem of frame dependence and violation of local Lorentz invariance in the usual formulation of f (T ) gravity is a consequence of neglecting the role of spin connection. We re-formulate f (T ) gravity starting, instead of the "pure-tetrad" teleparallel gravity, from the covariant teleparallel gravity, using both the tetrad and the spin connection as dynamical variables, resulting in the fully covariant, consistent, and frame-independent, version of f (T ) gravity, which does not suffer from the notorious problems of the usual, pure-tetrad, f (T ) theory. We present the method to extract solutions for the most physically important cases, such as the Minkowski, the FRW and the spherically-symmetric ones. We show that in the covariant f (T ) gravity we are allowed to use an arbitrary tetrad in an arbitrary coordinate system along with the corresponding spin connection, resulting always to the same physically relevant field equations.

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Section: Spherically Symmetric Geometrymentioning

confidence: 99%

The covariant formulation of f ( T ) gravity

Krššák

Saridakis

2016

Class. Quantum Grav.

315

251

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“…Recently, Abbas and his collaborations [46][47][48][49][50] have discussed the anisotropic compact star models in GR, ( ), ( ), and ( ) theories in diagonal tetrad case with Krori and Barua (KB) metric. Abbas et al [ ] have studied anisotropic strange star which corresponds to quintessence dark energy model with the help equation of state = , where 0 <…”

Section: It Has Been Seen In [ ] That Neutron Star Solution In ( ) Grmentioning

confidence: 99%

“…Many authors have worked on the matching condition to compare the exterior solution with the interior solution [10,47,49,51]. We correspond the exterior geometry with our interior solution, evoked by the Schwarzschild solution which is given by the line element…”

Section: Matching Conditionsmentioning

confidence: 99%

Anisotropic Quintessence Strange Stars in f(T) Gravity with Modified Chaplygin Gas

Saha

Debnath

2018

Advances in High Energy Physics

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In this paper, we study the existence of strange star in the background of ( ) modified gravity where is a scalar torsion. In KB metric space, we derive the equations of motion using anisotropic property within the spherically strange star with modified Chaplygin gas in the framework of modified ( ) gravity. Then we obtain many physical quantities to describe the physical status such as anisotropic behavior, energy conditions, and stability. By the matching condition, we calculate the unknown parameters to evaluate the numerical values of mass, surface redshift, etc., from our model to make comparison with the observational data. 2 Advances in High Energy Physics in ( ) gravity. Recently there are some static solutions which are spherically symmetric with charged source in ( ) theory [25]. The physical conditions have been studied [26] for the existence of astrophysical stars in ( ) theory after obtaining a large group of static perfect fluid solutions [27]. Capozziello et. al [ ] have shown that, instead of ( ) gravity, ( ) removes the singularities for the exact black hole solution in D-Dimensions. Wormhole solution has been studied under ( ) gravity by Sharif and Rani [ ]. ey have also investigated ( ) gravity for static wormhole solution to verify energy conditions [ ]. Again, for charged noncommutative wormhole solutions in f(T) gravity, Sharif and Rani [ , ] have seen that this solution exists by violating energy conditions.Generally, perfect fluid (isotropic fluid) inside the stellar object to study stellar structure and evolution is assumed because there exists isotropic pressure inside the fluid sphere. However, present observation shows that the fluid pressure of the highly compact astrophysical objects like X-ray pulsar, Her-X-, X-ray buster U -, millisecond pulsar SAXJ . -, etc. becomes anisotropy in nature which means the pressure can be rotten into two components such that one is radial pressure ( ) and the other is transverse pressure ( ). Now, Δ = − is known as the anisotropic factor. e anisotropy may arise for the different cases such as the existence of solid core, in presence of type P superfluid, phase transition, rotation, magnetic field, mixture of two fluids, and existence of external field. Generally, strange quark matter contains u, d, and s quarks. ere are two ways to classify the formation of strange matter [ ]. One way is the transformation of the quark hadron phase in the early universe and the other way is the reformation of neutron stars to strange matter at ultrahigh densities. A strange star is composed of the strange matter. Again the strange star can be classified into two types: Type I strange star with / > 0.3 and Type II strange star with 0.2 < / < 0.3. Depending on mass, radius, and energy density, the strange star is distinguished from the neutron star [ ]. It has been the most interesting topic to study the models of anisotropic stars for the last periods in GR and modified theories of gravity [35]. There have been many discussions about anisotropic star models in [36][37]...

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“…Thus, modified theories of gravity seem interesting in exploring the universe in different cosmological contexts [28]. The study of compact stars has always been a strong topic of research [29][30][31][32][33][34][35][36][37][38][39][40]. Different properties like mass, radius and moment of inertia of neutron stars are studied and a comparison has been developed with GR and alternative theories of gravity [41].…”

Section: Introductionmentioning

confidence: 99%

Physical attributes of anisotropic compact stars in f(R, G) gravity

Shamir

Zia

2017

Eur. Phys. J. C

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Modified gravity is one of the potential candidates to explain the accelerated expansion of the universe. Current study highlights the materialization of anisotropic compact stars in the context of f (R, G) theory of gravity. In particular, to gain insight in the physical behavior of three stars namely, Her X 1, SAX J 1808-3658 and 4U 1820-30, energy density, and radial and tangential pressures are calculated. The f (R, G) gravity model is split into a Starobinsky like f (R) model and a power law f (G) model. The main feature of the work is a 3-dimensional graphical analysis in which, anisotropic measurements, energy conditions and stability attributes of these stars are discussed. It is shown that all three stars behave as usual for positive values of the f (G) model parameter n.

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Anisotropic strange quintessence stars in f(T) gravity

Cited by 31 publications

References 41 publications

The covariant formulation of f ( T ) gravity

The covariant formulation of f ( T ) gravity

Anisotropic Quintessence Strange Stars in f(T) Gravity with Modified Chaplygin Gas

Physical attributes of anisotropic compact stars in f(R, G) gravity

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