A relativistic two-parameter core-envelope model of compact stars

Tikekar, Ramesh; Jotania, Kanti

doi:10.1134/s0202289309020042

Cited by 36 publications

(28 citation statements)

References 18 publications

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“…The anisotropy ∆ is increasing in the neighbourhood of the centre, reaches a maximum value and then subsquently decreases. The profile of ∆ is similar to the Sharma and Maharaj (2007) and the Tikekar and Jotania (2009) for strange stars with quark matter.…”

Section: Physical Featuressupporting

confidence: 84%

Compact models with regular charge distributions

Takisa

Maharaj

2012

Astrophys Space Sci

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We model a compact relativistic body with anisotropic pressures in the presence of an electric field. The equation of state is barotropic with a linear relationship between the radial pressure and the energy density. Simple exact models of the Einstein-Maxwell equations are generated. A graphical analysis indicates that the matter and electromagnetic variables are well behaved. In particular the proper charge density is regular for certain parameter values at the stellar centre unlike earlier anisotropic models in the presence of charge. We show that the electric field affects the mass of stellar objects and the observed mass for a particular binary pulsar is regained. Our models contain previous results of anisotropic charged matter with a linear equation of state for special parameter values.

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Section: Physical Featuressupporting

confidence: 84%

Compact models with regular charge distributions

Takisa

Maharaj

2012

Astrophys Space Sci

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“…Empirically, in order to design the core envelope model, the Darmois-Isreali conditions should be satisfied at the junction of the core and the envelope. With this empirical aspect, many authors [1,[12][13][14][15][16][17][18][19][20][21][22] have developed stellar models, with an assumption of a core and an envelope, for highly dense relativistic objects. Eventually in most of the core-envelope solutions so far obtained have the continuity of only metric potentials and pressure at the junction of the core and the envelope.…”

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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“…In (3+1) dimensions, the Finch and Skea [2] ansatz has been found to be useful to develop physically accept-able models capable of describing realistic stars. The physical 3-space of the back ground space-time, when embedded in a 4-dimensional Euclidean space, represents a 3-paraboloid which is a departure from the 3-spherical geometry [10], [11]. Similarly, in (2 + 1) dimensions, though the space-time remains circularly symmetric, the t = constant hyper-surface of the associated background space-time becomes a parabola rather than a circle.…”

Section: Introductionmentioning

confidence: 99%

Finch-Skea star in $$(2+1)$$ dimensions

et al. 2013

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The Bañados, Teitelboim and Zanelli[1] solution corresponding to the exterior space-time of a black hole in (2 + 1) dimensions has been found to be very useful to understand various aspects relating to the gravitational field of a black hole. We present here a class of interior solutions corresponding to the BTZ exterior by making use of a model presented by Finch and Skea[2] which was earlier found to be relevant for the description realistic stars in (3 + 1) dimensions. We show physical viability of the model in lower dimensions as well.

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A relativistic two-parameter core-envelope model of compact stars

Cited by 36 publications

References 18 publications

Compact models with regular charge distributions

Compact models with regular charge distributions

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

Finch-Skea star in $$(2+1)$$ dimensions

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