Abstract
We have presented a class of charged superdense star models, starting with a static spherically symmetric metric in isotropic coordinates for anisotropic fluid by considering Hajj-Boutros-(1986) type metric potential and a specific choice of electrical intensity E and anisotropy factor Δ which involve charge parameter K and anisotropy parameter α. The solution is well behaved for all the values of Schwarzschild compactness parameter u lying in the range 0<u≤0.2086, for all values of charge parameter K lying in the range 0.04≤K≤0.111 , and for all values of anisotropy parameter α lying in the range 0.016≥α≥0. With the increase in α, the values of K and u decrease. Further, we have constructed a superdense star model with all degree of suitability. The solution so obtained is utilized to construct the models for superdense star like neutron stars ρb=2.7×1014 g/cm3 and strange quark stars ρb=4.6888×1014 g/cm3 . For K=0.06 and α=0.01, the maximum mass of neutron star is observed as M=1.53 M⊙ and radius R=11.48 km. Further for strange quark stars M=1.16 M⊙ and R=8.71 km are obtained.
Highlights
Since the formulation of Einstein-Maxwell field equations, the relativists have been proposing different models of immensely gravitating astrophysical objects by considering the distinct nature of matter or radiation present in them
(iii) Bonnor [3] pointed out that a dust distribution of arbitrarily large mass and small radius can remain in equilibrium against the pull of gravity by a repulsive force produced by a small amount of charge
(viii) Ivanov [9] pointed out that solutions in isotropic coordinates are more significant than the solutions in curvature coordinates, due to the following reasons: (a) the solutions in isotropic coordinates are simple in terms of algebraic expressions; (b) isotropic coordinates solutions can be used as seed solutions in Quasar modeling or nonstatic solutions
Summary
Since the formulation of Einstein-Maxwell field equations, the relativists have been proposing different models of immensely gravitating astrophysical objects by considering the distinct nature of matter or radiation (energy-momentum tensor) present in them. For realistic model it is desirable to study the insinuation of Einstein-Maxwell field equations with reference to the general relativistic prediction of gravitational collapse with anisotropic matter. For this purpose charged fluid ball models are required. A considerable number of exact solutions with well-behaved nature of general relativistic field equation with anisotropic matter have been obtained; Dev and Gleiser [14], Komathiraj and Maharaj [15, 16], Thirukkanesh and Regel [17], Takisa and Maharaj [18, 19], Mak and Harko [20], Mak et al [21], Ivanov [1], Maurya and Gupta [22, 23], Chaisi and Maharaj [24], and Feroze and Siddiqui [25] deal with curvature coordinates and some of them are charged models. By motivation of Maharaj-Takisa [6] and Ivanov [9], in this paper, we present a new class of well-behaved exact solutions of Einstein-Maxwell field equations in isotropic coordinates for anisotropic fluid assuming a particular form of one of the metric potentials and suitable choice of electric intensity and anisotropy
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