Exact solutions: neutral and charged static perfect fluids with pressure

Bijalwan, Naveen

doi:10.1007/s10509-011-0834-3

Cited by 3 publications

(2 citation statements)

References 25 publications

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“…Tikekar [13] found an exact solution for a particular spheroidal geometry which could be used to model superdense neutron stars of densities in the range of 10 14 gcm −3 ; this solution has been generalized by Maharaj and Leach [14]. There have been extensive studies on charged spheroidal stars by considering a particular form for the electric field in recent years [15][16][17][18][19][20][21][22][23]. These charged spheroidal models contain uncharged neutron stars in the relevant limit and are consequently relevant in 2 Journal of Astrophysics the description of dense astrophysical objects.…”

Section: Introductionmentioning

confidence: 99%

New Classes of Charged Spheroidal Models

Thirukkanesh¹

2013

Journal of Astrophysics

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New classes of exact solutions to the Einstein-Maxwell system is found in closed form by assuming that the hypersurface is spheroidal. This is achieved by choosing a particular form for the electric field intensity. A class of solution is found for all positive spheroidal parameter for a specific form of electric field intensity. In general, the condition of pressure isotropy reduces to a difference equation with variable, rational coefficients that can be solved. Consequently, an explicit solution in series form is found. By placing restrictions on the parameters, it is shown that the series terminates and there exist two classes of solutions in terms of elementary functions. These solutions contain the models found previously in the limit of vanishing charge. Solutions found are directly relating the spheroidal parameter and electric field intensity. Masses obtained are consistent with the previously reported experimental and theoretical studies describing strange stars. A physical analysis indicates that these models may be used to describe a charged sphere.

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Section: Introductionmentioning

confidence: 99%

New Classes of Charged Spheroidal Models

Thirukkanesh¹

2013

Journal of Astrophysics

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“…Following this technique, a large number of solutions have been studied in [26][27][28][29][30]. In a recent treatment Naveen and Bijalwan [31,32] have obtained a charged perfect fluid model with generalized electric intensity for all K except for 0 < K < 1 and extending this point of view Kumar and Gupta [33,34] obtained another solution for 0 < K < 1. In the present problem we focused on a charged fluid sphere starting with Vaidya and Tikekar [1] metric potential and tested our model with some standard observed mass and radius of the compact stars candidates as proposed in [35].The paper is organized as follows: following a brief introduction in Sec.…”

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Charged Vaidya–Tikekar model for super compact star

et al. 2018

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In this work, we explore a class of compact charged objects that have been tested against experimental and observational constraints with some known compact stars candidates. This study is performed by considering the self-gravitating, charged, isotropic fluids which are more pliability in solving the Einstein-Maxwell equations. In order to determine the interior geometry, we utilize the VaidyaTikekar (J Astrophys Astron 3:325, 1982) geometry for the metric potential with Riessner-Nordström metric as an exterior solution. These model parameters are determined after selecting some particular values of M and R, for the compact objects SAX J1808.4-3658, Her X-1 and 4U 1538-52. The most striking consequence is that hydrostatic equilibrium is maintained for different forces, and the situation is clarified by using the generalized Tolman-Oppenheimer-Volkoff equation. In addition to this, we also present the energy conditions, speeds of sound and compactness of stars that are very much compatible to that for a physically acceptable stellar model. Arising solutions are also compared with graphical representations that provide strong evidences for more realistic and viable models, both at theoretical and astrophysical scale.

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A Nonsingular Perfect Fluid Classical Lepton Model of Arbitrarily Small Radius

Kiess¹

2013

Int. J. Mod. Phys. D

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We exhibit a classical lepton model based on a perfect fluid that reproduces leptonic charges and masses in arbitrarily small volumes without metric singularities or pressure discontinuities. This solution is the first of this kind to our knowledge, because to date the only classical general relativistic models that have reproduced leptonic charges and masses in arbitrarily small volumes are based on imperfect (anisotopic) fluids or perfect fluids with electric field discontinuities. We use a Maxwell–Einstein exact metric for a spherically symmetric static perfect fluid in a region in which the pressure vanishes at a boundary, beyond which the metric is of the Reissner–Nordström form. This construction models lepton mass and charge in the limit as the boundary → 0.

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Exact solutions: neutral and charged static perfect fluids with pressure

Cited by 3 publications

References 25 publications

New Classes of Charged Spheroidal Models

New Classes of Charged Spheroidal Models

Charged Vaidya–Tikekar model for super compact star

A Nonsingular Perfect Fluid Classical Lepton Model of Arbitrarily Small Radius

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