A family of well behaved charge analogues of Durgapal’s perfect fluid exact solution in general relativity

Abstract

This paper presents a new family of interior solutions of Einstein-Maxwell field equations in general relativity for a static spherically symmetric distribution of a charged perfect fluid with a particular form of charge distribution. This solution gives us wide range of parameter, K, for which the solution is well behaved hence, suitable for modeling of superdense star. For this solution the gravitational mass of a star is maximized with all degree of suitability by assuming the surface density equal to normal nuclear density, 2.5 10 kg m . By this model we obtain the mass of the Crab pulsar, , 1.3679 and radius 13.21 km, constraining the moment of inertia 1.61 10 kg m for the conservative estimate of Crab nebula mass 2 . And 1.9645 with radius 14.38 km constraining the moment of inertia 3.04 10 kg m for the newest estimate of Crab nebula mass, 4.6 . These results are quite well in agreement with the possible values of mass and radius of Crab pulsar. Besides this, our model yields moments of inertia for PSR J0737-3039A and PSR J0737-3039B, ! 1.4285 10 kg m and # 1.3647 10 kg m respectively. It has been observed that under well behaved conditions this class of solutions gives us the overall maximum gravitational mass of super dense object, &' () , 4.7487 with radius * + ,-. 15.24 km, surface redshift 0.9878, charge 7.91 10 / C, and central density 4.31 .

New charged anisotropic solution on paraboloidal spacetime

“…Since then, many researchers have studied the anisotropy Maharaj and Maartens [4], Gokhroo and Mehra [5], Patel and Mehta [6], Tikekar and Thomas [7], Tikekar and Thomas [8], Tikekar and Thomas [9], Thomas and Ratanpal [10], Dev and Gleiser [11], Dev and Gleiser [12], Dev and Gleiser [13] to name a few. A large number of researchers worked on Einstein's field equations, making different assumptions in the physical content as well as spacetime metric viz., Sharma and Ratanpal [14], Murad and Fatema [15], Murad and Fatema [16], Murad and Fatema [17], Pandya et al [18], Pandya and Thomas [19], Pandya and Thomas [20], Ratanpal et al [21].…”

Relativistic charged stellar modeling with a perfect fluid sphere

“…Also, the presence of the charge results in a greater bound for the rate between the mass M and radius R of the star u = GM/c 2 R [5-7] than the Buchdahl limit for the chargeless case [8], as such charged models result useful for explaining in an adequate manner the behaviour of massive objects as are Neutron stars, Pulsars and Quark stars. Some works that consider charged models have been applied to the description of compact objects like Crab Pulsar PSR B0531-21, the double pulsar system PSR J0737-3039 [9][10][11][12], the SAX J1808.4-3658 star [13], the star PSR J16142230, PSR J1903+327 and LMC X-4 [14,15]. Also, the effect of the charge has a notable relevance, to such degree that models with a perfect chargeless fluid, which are not physically acceptable as they are, can be electrified and when this occurs the results are models which are physically acceptable, in these cases, the form of the intensity of the electric field is important, an example of this is the interior Schwarzschild solution that does not meet the causality condition, but when it is electrified the causality condition is met, this particular case has the highest number of proposals of electrification [16][17][18][19][20][21][22][23].…”

Proposal of a Model of a Three-Dimensional Spherical Universe

“…The S 3 universe has a strong source of gravity in its center, and a part or all of it became a spacetime bubble where the universe was born [9]. The S 3 universe was explosively expanded by the Big Bang shortly after its birth, just like the current universe [9], eventually becoming a great sphere after the rate of expansion had slowed. Soon after, the S 3 universe started to contract gradually; the speed of the contraction increased until it finally contracted to the original origin (Figure 1) [9] [10].…”