Variety of Well behaved parametric classes of relativistic charged fluid spheres in general relativity

Abstract

The paper presents a variety of classes of interior solutions of Einstein-Maxwell field equations of general relativity for a static, spherically symmetric distribution of the charged fluid with well behaved nature. These classes of solutions describe perfect fluid balls with positively finite central pressure, positively finite central density; their ratio is less than one and causality condition is obeyed at the center. The outmarch of pressure, density, pressure-density ratio and the adiabatic speed of sound is monotonically decreasing for these solutions. Keeping in view of well behaved nature of these solutions, two new classes of solutions are being studied extensively. Moreover, these classes of solutions give us wide range of constant K for which the solutions are well behaved hence, suitable for modeling of super dense star. For solution (I 1 ) the mass of a star is maximized with all degree of suitability and by assuming the surface density ρ b = 2 × 10 14 g/cm 3 corresponding to K = 1.19 and X = 0.20, the maximum mass of the star comes out to be 2.5M with linear dimension 25.29 Km and central redshift 0.2802. It has been observed that with the increase of charge parameter K, the mass of the star also increases. For n = 4, 5, 6, 7, the charged solutions are well behaved with their neutral counterparts however, for n = 1, 2, 3, the charged solution are well behaved but their neutral counterparts are not well behaved.

New Class of Heintzmann Exact Solution in General Relativity for an Isotropic Charged Stellar Model

“…It is well known that, at the pressure free interface, the Reissner-Nordstrӧm solution is interesting to observe (present charge) the gravitational collapse of a spherical symmetric distribution of the matter to a point singularity may be avoided [1] if the matter distribution acquires large amount of electric charge. Any compact star is not composed of charged perfect fluid and may be used to make a suitable model of compact object with charge matter for the numerical study of the stellar structure [2,3,4].…”

Exact physical Maxwell-Einstein Tolman-VII solution and its use in stellar models

“…To date, several such metrics have been produced, but only the metric of Kuchowicz (1967) electrified in Gupta and Maurya (2011c), the Durgapal IV metric (1982) electrified in Pant (2011b), the Durgapal V metric (1982) electrified in Gupta and Maurya (2011b), and the two metrics of Pant (2011a) electrified in Maurya and Gupta (2011a) and Pant and Rajasekhara (2011) have been shown to satisfy all the above-mentioned physical constraints in the limit as Q → 0 (see Table 1). In these five electrified metrics, the coefficient of dt 2 (i.e., g tt in ds 2 = g tt dt 2 + g rr dr 2 + r 2 d 2 ) is by construction the same as in the chargeless case.…”

New class of Well behaved exact solutions of relativistic charged white-dwarf star with perfect fluid

“…Keeping in view of this aspect, several authors obtained the parametric class of exact solutions Cataldo and Mitskievic (1992), Ivanov (2002), Pant et al (2010Pant et al ( , 2011, Maurya (2010a, 2010b), Gupta (2011), Pant (2010), etc. These coupled solutions are well behaved with some positive values of charge parameter K and completely describe interior of the super-dense astrophysical object like White dwarf with charge matter.…”