Nature of the vorticity in the Gödel spacetime

Herrera, L.; Ibáñez, Jesús María Salinas; Prisco, A. Di

doi:10.1103/physrevd.87.087503

Cited by 21 publications

(24 citation statements)

References 25 publications

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“…For self-gravitating system, the polytropic equation plays a vital role. Polytropes with anisotropic matter distribution have widely been discussed in literature [36,37]. Here, we discuss two different cases related to the polytropes.…”

Section: Polytropic Equations With Vanishing Complexity Factormentioning

confidence: 97%

Complexity factor for charged spherical system

Sharif

Butt

2018

Eur. Phys. J. C

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In this paper, we study the complexity factor for a charged anisotropic self-gravitating object. We formulate the Einstein-Maxwell field equations, Tolman-Opphenheimer-Volkoff equation, and the mass function. We form the structure scalars by the orthogonal splitting of the Riemann tensor and then find the complexity factor with the help of these scalars. Finally, we investigate some astrophysical objects for the vanishing of complexity condition. It is found that the presence of the electromagnetic field decreases the complexity of the system.

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Section: Polytropic Equations With Vanishing Complexity Factormentioning

confidence: 97%

Complexity factor for charged spherical system

Sharif

Butt

2018

Eur. Phys. J. C

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“…[31,32]). From recent investigations of the stellar structure, Herrera and Barreto [33] considered polytropes for anisotropic matter both in the Newtonian and the GR regimes [34,35]. In [36,37], charged anisotropic solutions with a quadratic equation of state was obtained.…”

Section: Arxiv:191109546v1 [Gr-qc] 20 Nov 2019mentioning

confidence: 99%

Analytical model of dark energy stars

2020

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In this article we study the structure and stability of compact astrophysical objects which are ruled by the dark energy equation of state (EoS). The existence of dark energy is important for explaining the current accelerated expansion of the universe. Exact solutions to Einstein field equations (EFE) have been found by considering particularized metric potential, Finch and Skea ansatz [1]. The obtained solutions are relevant to the explanation of compact fluid sphere. Further, we have observed at the junction interface, the interior solution is matched with the Schwarzschild's exterior vacuum solution. Based on that, we have noticed the obtained solutions are well in agreement with the observed maximum mass bound of ≈ 2M , namely, PSR J1416-2230, Vela X-1, 4U 1608-52, Her X-1 and PSR J1903+327, whose predictable masses and radii are not compatible with the standard neutron star models. Also, the stability of the stellar configuration has been discussed briefly, by considering the energy conditions, surface redshift, compactness, mass-radius relation in terms of the state parameter (ω). Finally, we demonstrate that the features so obtained are physically acceptable and consistent with the observed/reported data [2,3]. Thus, the present dark energy equation of state appears talented regarding the presence of several exotic astrophysical matters.

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“…Eq (46) has been used in [56], [57], [58], [59], [60], [61], [62], [63], [64], [65], [66]. It is well-known that the Newtonian polytropes satisfy the non-linear Lane-Emden equation for perfect or anisotropic fluids [67]. It is integrable for just a few values of its parameter.…”

Section: Types Of Equationsmentioning

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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Nature of the vorticity in the Gödel spacetime

Cited by 21 publications

References 25 publications

Complexity factor for charged spherical system

Complexity factor for charged spherical system

Analytical model of dark energy stars

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

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