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

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In this paper, the spacetime geometry of Finch and Skea [Class. Quantum Grav. 6 (1989) 467] has been utilized to obtain closed-form solutions for a spherically symmetric anisotropic matter distribution. By examining its physical admissibility, we have shown that the class of solutions can be used as viable models for observed pulsars. In particular, a specific class of solutions can be used as an 'anisotropic switch' to examine the impact of anisotropy on the gross physical properties of a stellar configuration. Accordingly, the mass-radius relationship has been analyzed.

Section: Introductionmentioning

confidence: 99%

Anisotropic extension of Finch and Skea stellar model

Sharma¹,

Das²,

Thirukkanesh³

2017

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“…In particular, interior solutions corresponding to exterior BTZ spacetime have been developed and analyzed by Cruz and Zanelli (1995), Cruz et al (2005), Peixoto and Katanaev (2007), Sá (1999), Sharma et al (2011), García and Campuzano (2003), Banerjee et al (2013Banerjee et al ( , 2015, , Cataldo and Salgado (1996) and Garcia (2004). Recently, a non-commutative geometry inspired 3-dimensional charged black hole solution has been reported .…”

Section: Introductionmentioning

confidence: 99%

Gravitational collapse of a circularly symmetric star in an anti-de Sitter spacetime

Sharma¹,

Das²,

Rahaman

et al. 2015

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We investigate the collapse of a circularly symmetric star with outgoing radiation in (2 + 1)-dimensional anti-de Sitter spacetime. The exterior spacetime of the collapsing star is assumed to be described by the non-static generalization of the Bañados, Teitelboim and Zanelli [Phys. Rev. Lett. 69 (1992) 1849 ] metric. Making use of the junction conditions joining smoothly the interior and the exterior spacetimes across the boundary, we analyze the impacts of various factors on the evolution of the star which begins its collapse from an initial static configuration. In particular, depending on initial conditions, two possible outcomes of the collapse process are shown: (i) formation of a BTZ black hole; and (ii) evaporation of all mass-energy even before the singularity is reached.

“…García and Campuzano [7] have proposed a formalism to obtain circularly symmetric solutions from known density profile or EOS of the fluid source. Making use of Finch and Skea [8] ansatz in (2 + 1) dimensions, Banerjee et al [9] have generated new class of physically acceptable interior solutions corresponding to the BTZ exterior. Rahaman et al [10] have studied the properties of BTZ black hole by proposing new exact solutions of Einstein's field equations in (2 + 1) dimensional anti-de Sitter back ground space-time in the context of non-commutative geometry.…”

Section: Introductionmentioning

confidence: 99%

Exact solutions in (2+1)-dimensional anti-de Sitter space-time admitting a linear or non-linear equation of state

Banerjee

Rahaman

Jotania

et al. 2014

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Gravitational analyzes in lower dimensions has become a field of active research interest ever since Bañados, Teitelboim and Zanelli (BTZ) (Phys. Rev. Lett. 69, 1849Lett. 69, , 1992 proved the existence of a black hole solution in (2 + 1) dimensions. The BTZ metric has inspired many investigators to develop and analyze circularly symmetric stellar models which can be matched to the exterior BTZ metric. We have obtained two new classes of solutions for a (2 + 1)-dimensional anisotropic star in anti-de Sitter background space-time which have been obtained by assuming that the equation of state (EOS) describing the material composition of the star could either be linear or non-linear in nature. By matching the interior solution to the BTZ exterior metric with zero spin, we have demonstrated that the solutions provided here are regular and well-behaved at the stellar interior.