Newtonian polytropes for anisotropic matter: General framework and applications

Herrera, L.; Barreto, W.

doi:10.1103/physrevd.87.087303

Cited by 118 publications

(110 citation statements)

References 45 publications

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“…The equation (10) corresponds to a polytropic equation of state of the second class. Where the polytropic constant is α and the polytropic index (n) is infinity ,a particular case of equation (36) in reference (Herrera & Barreto 2013) Solving equations (6) − (8) with help of equations (9) and (10) one can obtain…”

Section: Interior Solutions and Einstein Field Equationmentioning

confidence: 99%

Singularity-free anisotropic strange quintessence star

Bhar

2014

Astrophys Space Sci

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Present paper provides a new model of anisotropic strange star corresponding to the exterior schwarzschild metric.The Einstein field equations have been solved by utilizing the Krori-Barua (KB) ansatz [K.D. Krori and J. Barua, J. Phys. A: Math. Gen. 8, 508 (1975)] in presence of quintessence field characterized by a parameter ω q with −1 < ω q < − 1 3 .The obtained solutions are free from central singularity. Our model is potentially stable.The numerical values of mass of the different strange stars SAXJ1808.4-3658(SS1)(radius=7.07 km),4U1820-30 (radius=10 km),Vela X-12 (radius=9.99 km),PSR J 1614-2230 (radius=10.3 km) obtained from our model is very close to the observational data that confirms the validity of our proposed model. The interior solution is also matched to the exterior Schwarzschild spacetime in presence of thin shell where negative surface pressure is required to hold the thin shell against collapse.

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Section: Interior Solutions and Einstein Field Equationmentioning

confidence: 99%

Singularity-free anisotropic strange quintessence star

Bhar

2014

Astrophys Space Sci

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“…1,2,45,46,[83][84][85] The first model is obtained by heuristic procedure which allows one to obtain solutions for anisotropic matter from known solutions for isotropic matter. 1,46 See more detail about the procedure used to get this model (HB) of q in Ref.…”

Section: ) (3) Beyond One Fluid Descriptionmentioning

confidence: 99%

Anisotropic pressure and hyperons in neutron stars

Sulaksono

2015

Int. J. Mod. Phys. E

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We study the effects of anisotropic pressure on properties of the neutron stars with hyperons inside its core within the framework of extended relativistic mean field. It is found that the main effects of anisotropic pressure on neutron star matter is to increase the stiffness of the equation of state, which compensates for the softening of the EOS due to the hyperons. The maximum mass and redshift predictions of anisotropic neutron star with hyperonic core are quite compatible with the result of recent observational constraints if we use the parameter of anisotropic pressure model h ≤ 0.8 1 and Λ ≤ −1.15. 2 The radius of the corresponding neutron star at M =1.4 M ⊙ is more than 13 km, while the effect of anisotropic pressure on the minimum mass of neutron star is insignificant. Furthermore, due to the anisotropic pressure in the neutron star, the maximum mass limit of higher than 2.1 M ⊙ cannot rule out the presence of hyperons in the neutron star core.

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“…There are also models with quadratic EOS and λ [100][101][102]. The popular polytropic EOS from Newtonian gravity was shown to lead in the anisotropic Newtonian case to the well-known LaneEmden equations [103] and to their relativistic generalisation in Einstein's gravity [104]. A simple solution for a simple ansatz for λ has been found [105].…”

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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Newtonian polytropes for anisotropic matter: General framework and applications

Cited by 118 publications

References 45 publications

Singularity-free anisotropic strange quintessence star

Singularity-free anisotropic strange quintessence star

Anisotropic pressure and hyperons in neutron stars

Analytical study of anisotropic compact star models

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