Stellar modelling of PSR J1614-2230 using the Karmarkar condition

Gedela, Satyanarayana; Bisht, Ravindra K.; Pant, Neeraj

doi:10.1140/epja/i2018-12637-8

Cited by 57 publications

(19 citation statements)

References 45 publications

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“…In recent past, many attempts have been made by various authors to find exact analytic solutions of the Einstein field system using linear EOS with MIT bag model [25][26][27][28][29][30][31] as well as quadratic EOS [32][33][34][35][36][37][38][39]. On the other hand, various authors [40][41][42][43][44][45] have also explored new solutions of the Einstein field equations for anisotropic fluid under the Karmarkar condition [46].…”

Section: Introductionmentioning

confidence: 99%

Core-envelope model of super dense star with distinct equation of states

2019

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The aim of the present paper is to study an anisotropic spherically symmetric core-envelope model of a super dense star in which core is equipped with linear equation of state, consistent with the quark matter while the envelope is considered to be of quadratic equation of state by adopting the philosophy of Takisa et al. (Pramana J Phys 92:40, 2019). We demonstrate that all the physical parameters are realistic within the core as well as envelope of the stellar object and continuous at the junction. Our model is shown to be physically viable and substantiate with the strange stars SAX J1808.4-3658 and 4U1608-52. Further, We infer that if the mass of the star increases then central density results to higher values and core shrinks, which justifies the dominating effect of gravity for higher mass celestial objects.

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Section: Introductionmentioning

confidence: 99%

Core-envelope model of super dense star with distinct equation of states

2019

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“…In relativistic stars, with anisotropic fluid distribution, the consideration is more perplex. The gamma is higher than the normal considered critical limit [63,64]. As a consequence, with increment of the charge, it is observed that the adiabatic index is also increases and hence the EOS of the stars becomes stiffer.…”

Section: (Iii) Adiabatic Indexmentioning

confidence: 86%

Charged anisotropic strange stars in Finslerian geometry

et al. 2019

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We investigate a simplified model of the strange stars in the framework of Finslerian geometry, composed of charged fluid. It is considered that the fluid consisting of three flavor quarks including a small amount of non-interacting electrons to maintain the chemical equilibrium and assumed that the fluid is compressible by nature. To obtain the simplified form of the charged strange star we have considered constant flag curvature. Based on geometry, we have developed the field equations within the localized charge distribution. We consider that the strange quarks distributed within the stellar system are complied with the MIT bag model type of equation of state (EOS) and the charge distribution within the system follows a power law. We represent the exterior spacetime by the Finslerian Ressiner-Nordström space-time. The maximum anisotropic stress is obtained at the surface of the system. Whether the system is in equilibrium or not, has been examined with respect to the Tolman-Oppenheimer-Volkoff (TOV) equation, Herrera cracking concept, different energy conditions and adiabatic index. We obtain that the total charge is of the order of 10 20 C and the corresponding electric field is of around 10 22 V/m. The central density and central pressure vary inversely with the charge. Varying the free parameter (charge constant) of the model, we find the generalized mass-radius variation of strange stars and determine the maximum limited mass with the corresponding radius. Furthermore, we also considered the variation of mass and radius against central density respectively.

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“…Karmarkar [37] developed a mandatory condition for a static and spherically symmetric line element to be of class one. In recent years, different researchers have considered the KMc to discussed the configurations of spherically symmetric compact objects [38][39][40][41][42]. Kuhfittig [43] developed wormhole geometry using KMc and shown that the embedding theory may provide the basis for a complete wormhole solution.…”

Section: Literature Surveymentioning

confidence: 99%

Traversable wormhole solutions in f(R) gravity via Karmarkar condition

Shamir

Fayyaz

2020

Eur. Phys. J. C

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Motivated by recent proposals of possible wormhole shape functions, we construct a wormhole shape function by employing the Karmarkar condition for static traversable wormhole geometry. The proposed shape function generates wormhole geometry that connects two asymptotically flat regions of spacetime and satisfies the required conditions. Further, we discuss the embedding diagram in three-dimensional Euclidean space to present the wormhole configurations. The main feature of current study is to consider three well-known f(R) gravity models, namely exponential gravity model, Starobinsky gravity Model and Tsujikawa f(R) gravity model. Moreover, we investigate that our proposed shape function provides the wormhole solutions with less (or may be negligible) amount of exotic matter corresponding to the appropriate choice of f(R) gravity models and suitable values of free parameters. Interestingly, the solutions obtained for this shape function generate stable static spherically symmetric wormhole structure in the context of non-existence theorem in f(R) gravity. This may lead to a better analytical representation of wormhole solutions in other modified gravities for the suggested shape function.

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Stellar modelling of PSR J1614-2230 using the Karmarkar condition

Cited by 57 publications

References 45 publications

Core-envelope model of super dense star with distinct equation of states

Core-envelope model of super dense star with distinct equation of states

Charged anisotropic strange stars in Finslerian geometry

Traversable wormhole solutions in f(R) gravity via Karmarkar condition

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