The dark energy star and stability analysis

Bhar, Piyali; Rahaman, Farook

doi:10.1140/epjc/s10052-015-3270-7

Cited by 76 publications

(77 citation statements)

References 27 publications

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“…Rahaman et al [13] and Shee et al [14] studied anisotropic stars with a nonstatic conformal vector, tangential pressures and a specified spacetime potential. Quintessence fields [15], gravastar models [16] and braneworld structures [17] have been analysed with a conformal symmetry. These studies show that the assumption of a conformal symmetry in spacetime is useful in studying exact solutions of field equations and astrophysical processes in stars.…”

Section: Introductionmentioning

confidence: 99%

Spherical conformal models for compact stars

et al. 2017

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We consider spherical exact models for compact stars with anisotropic pressures and a conformal symmetry. The conformal symmetry condition generates an integral relationship between the gravitational potentials. We solve this condition to find a new anisotropic solution to the Einstein field equations. We demonstrate that the exact solution produces a relativistic model of a compact star. The model generates stellar radii and masses consistent with PSR J1614-2230, Vela X1, PSR J1903+327 and Cen X-3. A detailed physical examination shows that the model is regular, well behaved and stable. The mass-radius limit and the surface red shift are consistent with observational constraints.

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Section: Introductionmentioning

confidence: 99%

Spherical conformal models for compact stars

et al. 2017

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“…Thus, Eqs (52, 56, 59, 60) may be considered as generating functions for spacetimes admitting conformal motion. Such solutions have been studied also in [81], [82], [83], [84], [85], [86], [87]. Conformally flat solutions are discussed in [88], [89], [90], [91], [92], [93].…”

Section: Spacetimes Admitting Conformal Motionmentioning

confidence: 99%

Linear and Riccati equations in generating functions for stellar models in general relativity

Иванов

2020

Eur. Phys. J. Plus

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It is shown that the expressions for the tangential pressure, the anisotropy factor and the radial pressure in the Einstein equations may serve as generating functions for stellar models. The latter can incorporate an equation of state when the expression for the energy density is also used. Other generating functions are based on the condition for the existence of conformal motion (conformal flatness in particular) and the Karmarkar condition for embedding class one metrics. In all these cases the equations are linear first order differential equations for one of the metric components and Riccati equations for the other. The latter may be always transformed into second order homogenous linear differential equations. These conclusions are illustrated by numerous particular examples from the study of stellar models.

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“…It is defined as [40,41,42] Using compactness factor the surface redshift is defined as (see [40,42] for details)…”

Section: Anisotropic Envelopementioning

confidence: 99%

Superdense star in a spacetime with minimal length

2019

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In this paper we generalise core-envelope model of superdense star to a non-commutative space-time and study the modifications due to the existence of a minimal length, predicted by various approaches to quantum gravity. We first derive Einstein's field equation in κdeformed space-time and use this to set up non-commutative version of core-envelope model describing superdense stars. We derive κdeformed law of density variation, valid upto first order approximation in deformation parameter and obtain radial and tangential pressures in κ-deformed space-time. We also derive κ-deformed strong energy conditions and obtain a bound on the deformation parameter. * bhanukiran.

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The dark energy star and stability analysis

Cited by 76 publications

References 27 publications

Spherical conformal models for compact stars

Spherical conformal models for compact stars

Linear and Riccati equations in generating functions for stellar models in general relativity

Superdense star in a spacetime with minimal length

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