Conformally flat charged dust

Banerjee, A.; Som, M. M.

doi:10.1007/bf00669526

Cited by 13 publications

(14 citation statements)

References 8 publications

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“…In addition to that, Sharma et al (2001) and Gupta and Kumar (2005b) have charged the Vaidya-Tikekar type solutions (Mukherjee et al 1997;Vaidya and Tikekar 1982) and Buchdahl's (1959) fluid spheres. Schwarzschild's solution also has been charged by Banerjee and Som (1981), Cohen et al (1969), Grøn (1985), Gupta et al (1986), Florides (1983), Guilfoyle (1999) and Gupta and Kumar (2005a). In this context the work by Maharaj and Komathiraj (2007a, 2007b, 2008, Maharaj and Thirukkanesh (2006a, 2006b, 2009), Maharaj and Hansraj (2006c), may also be visited.…”

mentioning

confidence: 89%

A class of charged analogues of Durgapal and Fuloria superdense star

Gupta

Maurya

2010

Astrophys Space Sci

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A class of charged analogues of superdense star model due to M.C. Durgapal and R.S. Fuloria, is obtained by using a particular electric field, which involves a parameter K. The members of this class are seen to satisfy the various physical conditions e.g. c 2 ρ ≥ 3p ≥ 0, dp/dr < 0, dρ/dr < 0, along with the velocity of sound condition dp/c 2 dρ < 1 and the adiabatic index ((p + c 2 ρ)/p)(dp/(c 2 dρ)) > 1 for the interval 1 < K ≤ 1.73 with the maximum mass 3.2860 M and the radius 18.3990 km.It is interesting to note that the velocity of sound and the ratio p/c 2 ρ are monotonically decreasing towards the pressure free interface for 1 < K ≤ 1.10216 which presents a relevant modelling for massive star like Neutron star or pulsar. In the interval 1 < K ≤ 1.10216, the maximum mass and the corresponding radius are given as 1.9672 M and 15.9755 km respectively.

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confidence: 89%

A class of charged analogues of Durgapal and Fuloria superdense star

Gupta

Maurya

2010

Astrophys Space Sci

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“…Kuchowicz (1968) solutions by Nduka (1977), Adler (1974)-Wyman (1949 solutions by Nduka (1976) and Singh and Yadav (1978), Klein (1947)-Tolman (1939 solutions by Pant and Sah (1979) Tikekar (1984) and Cataldo and Mitskievic (1992). In addition to that Sharma et al (2001), Gupta et al (2011) and Kumar (2005b, 2005c) charged the Vaidya-Tikekar type solutions (Mukherjee et al 1997;Vaidya and Tikekar 1982) and Buchdahl's (1959) fluid spheres. In this context the work by Maharaj and Komathiraj (2007a, 2007b, 2008, Maharaj and Thirukkanesh (2006a, 2006b, 2009).…”

Section: Charged Fluidsmentioning

confidence: 88%

“…Recently Maurya (2010a, 2010b) charged the Durgapal (1982), Durgapal and Fuloria (1985) Neeraj Pant et al (2010) charged the Heintzmann (1969) solutions. Schwarzchild's solution has also been charged by Banerjee and Som (1981), Cohen and Cohen (1969), Grøn (1985), Gupta and Gupta (1986), Florides (1983), Guilfoyle (1999) and Gupta and Kumar (2005a). All the solutions mentioned above are reducible to their neutral counterpart in the absence of charge.…”

Section: Charged Fluidsmentioning

confidence: 90%

A class of well behaved charged superdense star models of embedding class one

Gupta

Kumar

2011

Astrophys Space Sci

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A class of well behaved charged superdense star models of embedding class one is obtained by taking perfect fluid to be interior matter. In the process we come across the models for white dwarf, quark and neutron stars. Maximum mass of the star of this class is found to be 6.716998M with its radius is 18.92112 Km. In the absence of charge the models reduce to Schwarzchild's interior model with constant density.

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“…B. Griffiths [6][7][8][9]. In the present paper we shall investigate the properties of one class of solutions found by A. Banerjee and M. M. Som [10] and another one by S. N. Pandey and R. Tiwari [11]. We show that they are generalizations of the LBR solution.…”

Section: Introductionmentioning

confidence: 84%

Generalizations of the Levi-Civita-Bertotti-Robinson spacetime

Grøn

Johannesen

2014

Eur. Phys. J. Plus

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The Levi-Civita Bertotti Robinson (LBR) solution of Einstein's field equations may be interpreted to describe spacetime in a region without matter outside a charged spherical domain wall. In the present paper we investigate the physical properties of some solutions of the Einstein-Maxwell equations, and show that they are generalizations of the LBR solution. One represents a spacetime with charged dust outside a charged shell, and another one a spacetime with Lorentz Invariant Vacuum Energy (LIVE) outside a charged shell. The uniqueness of static, spherically symmetric and conformally flat solutions of the Einstein-Maxwell field equations is also discussed.

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Conformally flat charged dust

Cited by 13 publications

References 8 publications

A class of charged analogues of Durgapal and Fuloria superdense star

A class of charged analogues of Durgapal and Fuloria superdense star

A class of well behaved charged superdense star models of embedding class one

Generalizations of the Levi-Civita-Bertotti-Robinson spacetime

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