A class of charged analogues of Durgapal and Fuloria superdense star

Gupta, Yashwant; Maurya, S. K.

doi:10.1007/s10509-010-0445-4

Cited by 68 publications

(34 citation statements)

References 30 publications

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“…In connection to anisotropy we note that it was Ruderman [6] who argued that the nuclear matter may have anisotropic features at least in certain very high density ranges (>10 15 gm/cm 3 ), and thus the nuclear interaction can be treated under relativistic background. Later on Bowers and Liang [7] specifically investigated the non-negligible effects of anisotropy on the maximum equilibrium mass and surface redshift.…”

Section: Introductionmentioning

confidence: 86%

“…They showed that the model in connection to the neutron star stands all physical tests with the maximum mass 4.17 M and the surface redshift 0.63. Very recently, Gupta and Maurya [3] presented a class of charged analogs of the superdense star model due to Durgapal and Fuloria [1] with Einstein-Maxwell spacetimes. The members of this class have been shown to satisfy various physical conditions and exhibit these features: (a) a maximum mass 3.2860 M and a radius 18.3990 km for a particular interval of the parameter: 1 < K ≤ 1.7300, and (b) a maximum mass 1.9672 M and a radius 15.9755 km for another interval of the parameter: 1 < K ≤ 1.1021.…”

Section: Introductionmentioning

confidence: 99%

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Anisotropic models for compact stars

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In the present paper we obtain an anisotropic analog of the Durgapal and Fuloria (Gen Relativ Gravit 17:671, 1985) perfect fluid solution. The methodology consists of contraction of the anisotropic factor with the help of both metric potentials e ν and e λ . Here we consider e λ the same as Durgapal and Fuloria (Gen Relativ Gravit 17:671, 1985) did, whereas e ν is as given by Lake (Phys Rev D 67:104015, 2003). The field equations are solved by the change of dependent variable method. The solutions set mathematically thus obtained are compared with the physical properties of some of the compact stars, strange star as well as white dwarf. It is observed that all the expected physical features are available related to the stellar fluid distribution, which clearly indicates the validity of the model.

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Section: Introductionmentioning

confidence: 86%

Section: Introductionmentioning

confidence: 99%

Anisotropic models for compact stars

et al. 2015

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“…(iv) It is seen that the physical parameters like total mass, radius, mass to radius ratio, total charge to total mass ratio, central red shift and surface red shift increases with increasing β 1 (or f 0 ) and u, and decreasing L. (v) Interestingly, red-shift, velocity of sound and p/c 2 ρ are monotonically decreasing towards the pressurefree surface while adiabatic index is monotonically increasing. The velocity of sound and the ratio p/c 2 ρ monotonically decreasing towards the surface are also possessed by the uncharged model, Knutsen (1989) and charged model, Gupta and Maurya (2010). Energy density ρ and pressure p from (3.7) and (3.8) can be expressed in terms of parameters L and β 1 on using f 0 = 1+β 1 2R 2 and f a = (3L − 2)/(2R 2 ) from (2.5) and (3.5) respectively.…”

Section: Numerical Values Of Physical Quantitiesmentioning

confidence: 97%

Charged analogues of Schwarzschild interior solution in terms of pressure

Bijalwan

2011

Astrophys Space Sci

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Recently, Bijalwan (Astrophys. Space Sci., doi: 10.1007/s10509-011-0691-0, 2011a) discussed charged fluid spheres with pressure while Bijalwan and Gupta (Astrophys. Space Sci. 317, 251-260, 2008) suggested using a monotonically decreasing function f to generate all possible physically viable charged analogues of Schwarzschild interior solutions analytically. They discussed some previously known and new solutions for Schwarzschild parameter u(= GM c 2 a ) ≤ 0.142, a being radius of star. In this paper we investigate wide range of u by generating a class of solutions that are well behaved and suitable for modeling Neutron star charge matter. We have exploited the range u ≤ 0.142 by considering pressure p = p(ω) and2 to explore new class of solutions. Hence, class of charged analogues of Schwarzschild interior is found for barotropic equation of state relating the radial pressure to the energy density. The analytical models thus found are well behaved with surface red shift z s ≤ 0.181, central red shift z c ≤ 0.282, mass to radius ratio M/a ≤ 0.149, total charge to total mass ratio e/M ≤ 0.807 and satisfy Andreasson's (Commun. Math. Phys. 288, 715-730, 2009) stability condition. Red-shift, velocity of sound and p/c 2 ρ are monotonically decreasing towards the surface while adiabatic index is monotonically increasing. The maximum mass found to be 1.512 M with linear dimension 14.964 km. Class of charged analogues of Schwarzschild interior discussed in this paper doesn't have neutral counter part. These solutions completely describe interior of a stable Neutron star N. Bijalwan ( ) FreeLancer, c/o Sh. Rajkumar Bijalwan, Nirmal Baag, Part A,

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“…, [(n = 1) Tolman's IV (n = 2) Adler (1974), Heintzmann (1969), (n = 4, 5) Durgapal (1982), Gupta and Maurya (2010a), (n = 6) Pant et al (2010b)] Only solution by Gupta and Maurya (2010a) has well behaved neutral counterpart = e nω = e n(c 1 +c 2 r 2 ) Z =…”

Section: Physical Analysis Of the Solutionsmentioning

confidence: 99%

Exact solutions: neutral and charged static perfect fluids with pressure

Bijalwan¹

2011

Astrophys Space Sci

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We show in this article that charged fluid with pressure derived by Bijalwan (Astrophys. Space. Sci. , 2011a) can be used to model classical electron, quark, neutron stars and pulsar with charge matter, quasi black hole, white dwarf, super-dense star etc. Recent analysis by Bijalwan (Astrophys. Space. Sci., 2011d) that all charged fluid solutions in terms of pressure mimic the classical electron model are partially correct because solutions by Bijalwan (Astrophys. Space. Sci. ) may possess a neutral counterpart. In this paper we characterized solutions in terms of pressure for charged fluids that have and do not have a well behaved neutral counter part considering same spatial component of metric e λ for neutral and charged fluids. We discussed solution by Gupta and Maurya (Astrophys. Space Sci. 331(1):135-144, 2010a) and solutions by Bijalwan (Astrophys. Space Sci. , 2011c; Astrophys. Space Sci., 2011d) such that charged fluids possess and do not possess a neutral counterpart as special cases, respectively. For brevity, we only present some analytical results in this paper.

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A class of charged analogues of Durgapal and Fuloria superdense star

Cited by 68 publications

References 30 publications

Anisotropic models for compact stars

Anisotropic models for compact stars

Charged analogues of Schwarzschild interior solution in terms of pressure

Exact solutions: neutral and charged static perfect fluids with pressure

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