Modified Finch and Skea stellar model compatible with observational data

Pandya, D. M.; Thomas, V. O.; Sharma, Ranjan

doi:10.1007/s10509-014-2207-1

Cited by 75 publications

(51 citation statements)

References 43 publications

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“…The anisotropic solution constructed depends of two parameters (n, w) which intervals is determinated for the relations (25) and (26) with A given by (27). The specific values of these parameters fix the type of compact object that represent and this is given by the compacity ratio that can be determinated considering the form known for A and imposing the metric that must be continuous at the frontier, we get the the compactness ratios…”

Section: Compact Starsmentioning

confidence: 99%

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On the effect of anisotropy on stellar models

Estevez-Delgado

2018

Eur. Phys. J. C

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The relevance of anisotropy in compact models is shown by the construction of a stellar model, this can influence the behavior of density, pressure and speed of sound in such grade that if the anisotropy disappear it could produce a regular model of perfect fluid which is not physically acceptable. The present anisotropic model has dependence in two parameters n associated with the anisotropy and w related with the rate of compactness u = G M/c 2 R, this is regular and physically acceptable. That is the speed of sound is positive and lower than the light speed, the density as well as radial and tangential pressure are monotonic decrescent functions. The compactness values for which the radial and tangential speed of sound are monotonic decrescent functions and the solution is potentially stable occurs for u ≤ 0.2073450586, and in particular for the maximum value of u n ∈ [−0.771108398, −0.231572621]. While if n = 1 we get a model of perfect regular fluid but the density and speed of sound can not be both positive at the origin, so the solution is not physically acceptable in the absence of anisotropic pressures.

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Section: Compact Starsmentioning

confidence: 99%

“…Some of the anisotropic exact regular solutions which are physically acceptable were built from a regular solution of a perfect fluid with an additional anisotropic parameter which allows recover the solution for the perfect fluid [26][27][28], even though anisotropic solutions which has no similar for a perfect fluid exist [29][30][31].…”

Section: Introductionmentioning

confidence: 99%

On the effect of anisotropy on stellar models

Estevez-Delgado

2018

Eur. Phys. J. C

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“…Recently, solutions with prescribed λ and p r have been given full physical analysis [71][72][73][74]. At first sight, these are hybrid solutions, but since λ is closely related to ρ, we mention them here.…”

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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“…In this way we can model relativistic compact objects including dark energy stars, quark stars, gravastars, neutron stars and ultradense matter. For some recent models investigating the properties of charged anisotropic stars see the treatments of Feroze and Siddiqui [1], Thirukkanesh and Ragel [2], Maurya and Gupta [3], Maurya et al [4], Pandya et al [5], Bhar et al [6] and Murad [7].…”

Section: Introductionmentioning

confidence: 99%

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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Modified Finch and Skea stellar model compatible with observational data

Cited by 75 publications

References 43 publications

On the effect of anisotropy on stellar models

On the effect of anisotropy on stellar models

Analytical study of anisotropic compact star models

New charged anisotropic compact models

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