Compact stars on pseudo-spheroidal spacetime compatible with observational data

Thomas, V. O.; Pandya, D. M.

doi:10.1007/s10509-015-2573-3

Cited by 9 publications

(4 citation statements)

References 38 publications

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“…20, which contains p r , y and a 1 , is the simplest generating function for any of them, when the other two are known. Solutions with given y (or m) and p r may be found in [17][18][19][20][21].…”

Section: The Energy Density and The Radial Pressurementioning

confidence: 99%

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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Section: The Energy Density and The Radial Pressurementioning

confidence: 99%

Generating solutions for charged stellar models in general relativity

Иванов

2021

Eur. Phys. J. C

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“…Sharma and Ratanpal (2013) described a quadratic equation of state in Finch Skea spacetime, a sub-class of the model described subsequently by Pandya et al (2015). A comprehensive report of compact stars on pseudo spheroidal spacetime compatible with observational data was provided by Thomas and Pandya (2015) .…”

Section: Introductionmentioning

confidence: 95%

Anisotropic compact star model satisfying Karmarkar conditions

Pandya

Thakore

Goti

et al. 2020

Astrophys Space Sci

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A new class of solutions describing the composition of compact stars has been proposed, assuming that the fluid distribution inside the star is anisotropic. This is achieved by assuming the appropriate metric potential and then solving Einstein's field equations using Karmarkar conditions [Karmarkar K. R., Proc. Indian Acad. Sci. 27 (1948) 56] to derive the expressions for star density, the radial and tangential pressures in terms of the constants A, B, a paramter 'a' and the curvature parameter R. The equations thus obtained have been passed through rigorous conditional analysis. It is further shown that the model is physically viable and mathematically well-behaved, fulfilling the requisite conditions viz., regularity condition, strong energy condition, causality condition, etc. Observed star candidates including EXO 1785-248, SMC X-1, SAXJ1808.43658(SS2), HER X-1, 4U 1538-52, Cen X-3 and LMC X-4 were found to conform to a good approximation through the outcome of this model for a=0.5.

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“…Since then, many researchers have studied the anisotropy Maharaj and Maartens [4], Gokhroo and Mehra [5], Patel and Mehta [6], Tikekar and Thomas [7], Tikekar and Thomas [8], Tikekar and Thomas [9], Thomas and Ratanpal [10], Dev and Gleiser [11], Dev and Gleiser [12], Dev and Gleiser [13] to name a few. A large number of researchers worked on Einstein's field equations, making different assumptions in the physical content as well as spacetime metric viz., Sharma and Ratanpal [14], Murad and Fatema [15], Murad and Fatema [16], Murad and Fatema [17], Pandya et al [18], Pandya and Thomas [19], Pandya and Thomas [20], Ratanpal et al [21].…”

Section: Introductionmentioning

confidence: 99%

New charged anisotropic solution on paraboloidal spacetime

Patel

Ratanpal

Pandya

2023

Preprint

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New exact solutions of Einstein's field equations for charged stellar models by assuming linear equation of state $ P_r=A(\rho-\rho_{a}) $, where $ P_r $ is the radial pressure and $ \rho_{a} $ is the surface density. By assuming $ e^{\lambda} = 1+\frac{r^2}{R^2} $ for metric potential. The physical acceptability conditions of the model are investigated, and the model is compatible with several compact star candidates like 4U 1820-30, PSR J1903+327, EXO 1785-248, Vela X-1, PSR J1614-2230, Cen X-3. A noteworthy feature of the model is that it satisfies all the conditions needed for a physically acceptable model.

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Compact stars on pseudo-spheroidal spacetime compatible with observational data

Cited by 9 publications

References 38 publications

Generating solutions for charged stellar models in general relativity

Generating solutions for charged stellar models in general relativity

Anisotropic compact star model satisfying Karmarkar conditions

New charged anisotropic solution on paraboloidal spacetime

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