A new solution of embedding class I representing anisotropic fluid sphere in general relativity

Singh, Ksh. Newton; Bhar, Piyali; Pant, Neeraj

doi:10.1142/s0218271816500991

Cited by 55 publications

(21 citation statements)

References 41 publications

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“…However, a very recently Bhar et al 22 and Maurya et al [23][24][25] have investigated an anisotropic compact star model of embedding class one. Some other notable works in this field have been done extensively by Singh et al [26][27][28][29][30][31] The paper has been divided in the following sections; in section 2 the field equations have been solved using the Karmakar condition.In section 3 a particular model have been discussed, next in section 4 we have worked on various physical acceptability conditions has must satisfied by our model. The exterior space-time and boundary conditions have been investigated in section 5.…”

Section: Introductionmentioning

confidence: 99%

A new class of relativistic model of compact stars of embedding class I

Bhar¹,

Singh

Manna

2017

Int. J. Mod. Phys. D

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In the present paper we have constructed a new relativistic anisotropic compact star model having a spherically symmetric metric of embedding class one. Here we have assumed an arbitrary form of metric function e λ and solved the Einstein's relativistic field equations with the help of Karmarkar condition for an anisotropic matter distribution. The physical properties of our model such as pressure, density, mass function, surface red-shift, gravitational red-shift are investigated and the stability of the stellar configuration is discussed in details. Our model is free from central singularities and satisfies all energy conditions. The model we present here satisfy the static stability criterion i.e. dM/dρc > 0 for 0 ≤ ρc ≤ 4.04 × 10 17 g/cm 3 (stable region) and for ρc ≥ 4.04 × 10 17 g/cm 3 , the region is unstable i.e., dM/dρc ≤ 0.

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Section: Introductionmentioning

confidence: 99%

A new class of relativistic model of compact stars of embedding class I

Bhar¹,

Singh

Manna

2017

Int. J. Mod. Phys. D

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“…Dev and Gleiser [16] proposed several exact solutions for anisotropic stars by taking constant density. We have extensively studied the charged and uncharged model of compact stars in some of our earlier works [17][18][19][20][21][22][23][24][25][26]. To find the exact solution, a more systematic approach is to assume conformal symmetry of the space-time.…”

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confidence: 99%

Effect of electric charge on anisotropic compact stars in conformally symmetric spacetime

et al. 2018

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We obtain a new class of interior solutions for charged anisotropic stars which admits non-static conformal motion. The Einstein-Maxwell field equations are solved by taking a physically reasonable choice for the g rr metric co-efficient and a suitable expression for charge density. From the analysis we have shown that there is a central singularity on space-time by calculating Kretschmann scalar though the central density and central pressure are finite. The emphasis are given on the causality condition and the stability analysis of the model. The masses and radii of the compact stars PSR J16142230, PSR J1903+327 and LMC X-4 obtained from the model are well match with the observed values provided by Gangopadhyay et al (2013 Mon. Not. R. Astron. Soc. 431 3216)

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“…For the choice of mass function gives a monotonic decreasing matter density as used earlier by Singh et al [31], for modelling a compact star of embedding class I. It will be suitable to express the physical variables in terms of metric function, and our anisotropic fluid configuration to be physically acceptable.…”

Section: Interior Space-time and The Field Equationsmentioning

confidence: 99%

Dark energy stars: Stable configurations

et al. 2018

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In present paper a spherically symmetric stellar configuration has been analyzed by assuming the matter distribution of the stellar configuration is anisotropic in nature and compared with the realistic objects, namely, the low mass X-ray binaries (LMXBs) and X-ray pulsars. The analytic solution has been obtained by utilizing the dark energy equation of state for the interior solution corresponding to the Schwarzschild exterior vacuum solution at the junction interface. Several physical properties like energy conditions, stability, mass-radius ratio, and surface redshift are described through mathematical calculations as well as graphical plots. It is found that obtained mass-radius ration of the compact stars candidates like 4U 1820-30, PSR J 1614-2230, Vela X-1 and Cen X3are very much consistent with the observed data by Gangopadhyay et al. (Mon. Not. R. Astron. Soc. 431, 3216 (2013)). So our proposed model would be useful in the investigation of the possible clustering of dark energy.

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A new solution of embedding class I representing anisotropic fluid sphere in general relativity

Cited by 55 publications

References 41 publications

A new class of relativistic model of compact stars of embedding class I

A new class of relativistic model of compact stars of embedding class I

Effect of electric charge on anisotropic compact stars in conformally symmetric spacetime

Dark energy stars: Stable configurations

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