A parametric model to study the mass–radius relationship of stars

Islam, Safiqul; Datta, Satadal; Das, Tapas K.

doi:10.1007/s12043-018-1704-0

Cited by 4 publications

(4 citation statements)

References 50 publications

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“…This is an expression for a 1 when y and l are given and was used for concrete ansatze in [31][32][33][34][35][36][37][38][39].…”

Section: The Energy Density and The Radial Pressurementioning

confidence: 99%

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Generating solutions for charged stellar models in general relativity

Иванов

2021

Eur. Phys. J. C

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It is shown that the expressions for the tangential pressure, the anisotropy factor and the radial pressure in the Einstein–Maxwell equations may serve as generating functions for charged 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, which do not depend on charge. 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 charged stellar models.

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“…This is an expression for a 1 when y and l are given and was used for concrete ansatze in [31][32][33][34][35][36][37][38][39].…”

Section: The Energy Density and The Radial Pressurementioning

confidence: 99%

“…+2z dr dr . (38) The generating potentials are Δ, z and l, the second, due to Eq (31), is equivalent to a 1 . This generating function encompasses the important cases of charged perfect fluid when Δ = 0 [40] and neutral perfect fluid when Δ = 0, l = 0.…”

Section: The Tangential Pressure and The Anisotropic Factormentioning

confidence: 99%

Generating solutions for charged stellar models in general relativity

Иванов

2021

Eur. Phys. J. C

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“…al. [125], Maharaj and Chaisi [126], the study of Thirukkanesh and Maharaj [129] on a charged anisotropic matter, and the investigations by Takisa and Maharaj [131] and Islam et al [132,138] on compact models with regular charge distribution.…”

Section: Solutions When An Equation Of State Is Assumedmentioning

confidence: 99%

The classification of interior solutions of anisotropic fluid configurations

Kumar¹,

Bharti²

2021

Preprint

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The solutions of the Einstein-Maxwell system of equations, useful for the modeling of compact stars have a long and rich history. It took just a year since Einstein's general theory of relativity was published for Karl Schwarzschild to obtain the first exact solution of Einstein's field equations. The number of viable exact solutions has been growing since then. Different models have been constructed for a variety of applications. In this article, we have discussed different ways of generating a static spherically symmetric anisotropic fluid model. The purpose of the present article is to present a simple classification scheme for static and spherically symmetric anisotropic fluid solutions. The known solutions are reviewed and compartmentalized according to this scheme so that we can illustrate general ideas about these solutions without being exhaustive.

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“…where n and 𝜌 𝑠 are constants. By approximating EOS in equation (44) to plot in figure (8), we obtain n = 0.081 and 𝜌 𝑠 = 0.022. The equation has not been derived through a priori assumptions of linearity or compliance to a certain curve.…”

Section: Approximated Equation Of Statementioning

confidence: 99%

A New Class of Analytical Solutions Describing Anisotropic Neutron Stars in General Relativity

Solanki,

Thakore

2021

Preprint

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A new class of solutions describing analytical solutions for compact stellar structures has been developed within the tenets of General Relativity. Considering the inherent anisotropy in compact stars, a stable and causal model for realistic anisotropic neutron stars was obtained using the general theory of relativity. Assuming a physically acceptable non-singular form of one metric potential and radial pressure containing the curvature parameter 𝑅, the constant 𝑘, and the radius 𝑟, analytical solutions to Einstein's field equations for anisotropic matter distribution were obtained. Taking the value of 𝑘 as -0.44, it was found that the proposed model obeys all necessary physical conditions, and it is potentially stable and realistic. The model also exhibits a linear equation of state, which can be applied to describe compact stars.

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A parametric model to study the mass–radius relationship of stars

Cited by 4 publications

References 50 publications

Generating solutions for charged stellar models in general relativity

Generating solutions for charged stellar models in general relativity

The classification of interior solutions of anisotropic fluid configurations

A New Class of Analytical Solutions Describing Anisotropic Neutron Stars in General Relativity

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