A class of relativistic stars with a linear equation of state

Sharma, Ranjan; Maharaj, S. D.

doi:10.1111/j.1365-2966.2006.11355.x

Cited by 231 publications

(179 citation statements)

References 35 publications

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“…In this section we generate stellar masses which are consistent with the results of Sharma and Maharaj [26], Thirukkanesh and Maharaj [21], and Mafa Takisa and Maharaj [22].…”

Section: Stellar Massessupporting

confidence: 67%

New charged anisotropic compact models

Matondo

Maharaj

2016

Astrophys Space Sci

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We find new exact solutions to the Einstein-Maxwell field equations which are relevant in the description of highly compact stellar objects. The relativistic star is charged and anisotropic with a quark equation of state. Exact solutions of the field equations are found in terms of elementary functions. It is interesting to note that we regain earlier quark models with uncharged and charged matter distributions. A physical analysis indicates that the matter distributions are well behaved and regular throughout the stellar structure. A range of stellar masses are generated for particular parameter values in the electric field. In particular the observed mass for a binary pulsar is regained.

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“…In this section we generate stellar masses which are consistent with the results of Sharma and Maharaj [26], Thirukkanesh and Maharaj [21], and Mafa Takisa and Maharaj [22].…”

Section: Stellar Massessupporting

confidence: 67%

New charged anisotropic compact models

Matondo

Maharaj

2016

Astrophys Space Sci

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“…[45,56,[67][68][69][70]82,95,99,100,102,105,106]. Models with such LEOS are discussed in [65,[93][94][95][96][97][98][99]. Obviously p r 0 = β (ρ 0 − ρ s ) > 0, p rs = 0.…”

Section: Solutions With Linear Eos and Simple Energy Densitymentioning

confidence: 99%

“…There are models with in addition given m, [93,94] or λ [95][96][97][98][99]. There are also models with quadratic EOS and λ [100][101][102].…”

Section: Introductionmentioning

confidence: 99%

Analytical study of anisotropic compact star models

Иванов

2017

Eur. Phys. J. C

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A simple classification is given of the anisotropic relativistic star models, resembling the one of charged isotropic solutions. On the ground of this database, and taking into account the conditions for physically realistic star models, a method is proposed for generating all such solutions. It is based on the energy density and the radial pressure as seeding functions. Numerous relations between the realistic conditions are found and the need for a graphic proof is reduced just to one pair of inequalities. This general formalism is illustrated with an example of a class of solutions with linear equation of state and simple energy density. It is found that the solutions depend on three free constants and concrete examples are given. Some other popular models are studied with the same method.

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“…Anisotropy in pressure could significantly affect the physical parameters like maximum compactness, mass and radius of star. A large number of anisotropic models are available in the literature [22]- [35]. Local anisotropy in self-gravitating systems were studied by Herrera & Santos [36] They conjectured that an anisotropic model can be stable.…”

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confidence: 99%

A New Charged Anisotropic Compact Star Model in General Relativity

Tamta¹,

Fuloria²

2017

JMP

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In the present article, we explore a new static, spherically symmetric charged anisotropic fluid model of compact star in curvature coordinates. We consider metric potential 44 g of Durgapal's fifth solution [1] with a specific choice of electric field intensity E and physically acceptable expression of anisotropy factor ∆ , which involve parameters K (charge) and ∆ (anisotropy) respectively. The solution so obtained is utilized to construct the model for super-dense star like neutron star. We have analysed that corresponding toand by assuming surface density 14 3 2 10 gm cm b ρ = × , the mass of the compact star comes out to be 2.17M Θ with radius 14.51 kms, which closely resembles to that of PSRJ0348 + 0432. The solution is well behaved for the values of K satisfying 1 5 K ≤ < . Our model is described analytically as well as with the help of graphical representations. Our solution is well behaved and free from any central singularity. It also satisfies all the energy conditions as well as the causality condition thus reconfirming the stability of our model.

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A class of relativistic stars with a linear equation of state

Cited by 231 publications

References 35 publications

New charged anisotropic compact models

New charged anisotropic compact models

Analytical study of anisotropic compact star models

A New Charged Anisotropic Compact Star Model in General Relativity

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