Gravastar solutions with continuous pressures and equation of state

DeBenedictis, Andrew; Horvat, Daniela; Ilijić, Saša; Kloster, S.; Viswanathan, K. S.

doi:10.1088/0264-9381/23/7/007

Cited by 153 publications

(137 citation statements)

References 39 publications

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“…The equation of state used for p r (ρ) serves here only as a closure relation and is therefore chosen to be in the simplest possible form, namely a polynomial of the type [10,15] …”

Section: A Rotating Gravastar Modelmentioning

confidence: 99%

“…Also an effort has been made to assess the properties of gravastars when these are perturbed [10,11]. The result of this analysis has lead, among other things, to the evidence that perturbations in spherical gravastars can be used to discriminate them from black holes, thus removing one of the most serious consequences of the existence of such ultra-compact objects [11].…”

Section: Introductionmentioning

confidence: 99%

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Ergoregion instability in rotating gravastars

2008

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The ergoregion instability is known to affect very compact objects that rotate very rapidly and do not possess a horizon. We present here a detailed analysis on the relevance of the ergoregion instability for the viability of gravastars. Expanding on some recent results, we show that not all rotating gravastars are unstable. Rather, stable models can be constructed also with J/M 2 ∼ 1, where J and M are the angular momentum and mass of the gravastar, respectively. The genesis of gravastars is still highly speculative and fundamentally unclear if not dubious. Yet, their existence cannot be ruled out by invoking the ergoregion instability. For the same reason, not all ultra-compact astrophysical objects rotating with J/M 2 1 are to be considered necessarily black holes.

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“…The equation of state used for p r (ρ) serves here only as a closure relation and is therefore chosen to be in the simplest possible form, namely a polynomial of the type [10,15] …”

Section: A Rotating Gravastar Modelmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Ergoregion instability in rotating gravastars

2008

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“…Selfbound systems composed of scalar fields, i.e., the 'boson stars' are naturally anisotropic [17]. Similarly, wormholes [18] and gravastars [19,20] are also structurally anisotropic systems. The shearing motion of the fluid is another source of anisotropy in self-gravitating objects [21][22][23].…”

Section: Introductionmentioning

confidence: 99%

Anisotropic generalization of well-known solutions describing relativistic self-gravitating fluid systems: an algorithm

Thirukkanesh¹,

Ragel

Sharma³

et al. 2018

Eur. Phys. J. C

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We present an algorithm to generalize a plethora of well-known solutions to Einstein field equations describing spherically symmetric relativistic fluid spheres by relaxing the pressure isotropy condition on the system. By suitably fixing the model parameters in our formulation, we generate closed-form solutions which may be treated as an anisotropic generalization of a large class of solutions describing isotropic fluid spheres. From the resultant solutions, a particular solution is taken up to show its physical acceptability. Making use of the current estimate of mass and radius of a known pulsar, the effects of anisotropic stress on the gross physical behaviour of a relativistic compact star is also highlighted.

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“…Scalar field 'boson stars' are naturally anisotropic (Schunch (2003)). Wormholes (Morris and Thorne (1988)) and gravastars (Cattoen et al (2005); DeBenedictis et al (2006)) have also anisotropic characteristics. Ivanov (2010) has pointed out that incorporation of the electromagnetic field into a relativistic stellar object has an anisotropic interpretation.…”

Section: Introductionmentioning

confidence: 99%

Anisotropic extension of Finch and Skea stellar model

Sharma¹,

Das²,

Thirukkanesh³

2017

Astrophys Space Sci

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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.

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Gravastar solutions with continuous pressures and equation of state

Abstract: We study the gravitational vacuum star (gravastar) configuration as proposed by [1] in a model where the interior de Sitter spacetime segment is continuously extended to the exterior Schwarzschild spacetime.

Cited by 153 publications

References 39 publications

Ergoregion instability in rotating gravastars

Ergoregion instability in rotating gravastars

Anisotropic generalization of well-known solutions describing relativistic self-gravitating fluid systems: an algorithm

Anisotropic extension of Finch and Skea stellar model

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