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 which involve charge parameter K and anisotropy parameter . The solution is well behaved for all the values of Schwarzschild compactness parameter u lying in the range , for all values of charge parameter K lying in the range , and for all values of anisotropy parameter lying in the range . With the increase in , 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 and strange quark stars . For and , the maximum mass of neutron star is observed as and radius . Further for strange quark stars and are obtained. 1. Introduction 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. Einstein-Maxwell field equations with anisotropic matter in isotropic coordinates have more importance over Einstein field equations for perfect fluid in curvature coordinates due to following rationale justifications.(i)The presence of some charge may avert the catastrophic gravitational collapse by counterbalancing the gravitational attraction by the electric repulsion in addition to the pressure gradient.(ii)The inclusion of charge inhibits the growth of space time curvature which has a great role in avoiding singularities (Ivanov [1]; de Felice et al. [2]).(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.(iv)The solutions of Einstein-Maxwell equations are useful to study the cosmic matter.(v)The charge dust models and electromagnetic mass models are providing some clue about the structure of electron (Bijalwan [4]) and Lepton model (Kiess [5]).(vi)Several solutions which do not satisfy some or all the conditions for well-behaved nature can be renewed into well-behaved nature by charging them.(vii)Maharaj-Takisa [6] pointed out that the astrophysical objects have essential characteristics of rotational motion, which is caused by the presence of anisotropic parameter. Therefore,
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