A charged perfect fluid solution

Abstract

A static and spherically symmetric stellar model is described by a perfect charged fluid. Its construction is done using the solution of the Einstein–Maxwell equations for which we specify the temporal metric and the electric field which is a monotonic increasing function null in the center. The density, pressure and speed of sound turn out to be regular functions, positive and monotonic decreasing as function of the radial distance. Also, the speed of sound is lower than the speed of light, that is to say, it does not violate the condition of causality. The value of compactness [Formula: see text], so the model is useful to represent neutron stars of quark stars. In a complementary manner, we report the physical values when describing a star of mass [Formula: see text] and radius [Formula: see text], in such case [Formula: see text], and given the presence of the charge, the interval for the central density [Formula: see text].

Relativistic charged stellar modeling with a perfect fluid sphere

“…There are several ways in which we can obtain a solution to Einstein's equations with a charged perfect fluid. One of them which is important, and that allows to generalize an existing physically acceptable solution for the chargeless case to the charged case, consists in taking one of the metric potentials g tt or g rr which corresponds to a solution with perfect fluid and solve the equations system (3)-( 5) assuming an appropriate form for the electric field's intensity [81][82][83][84][85][86][87]. And although, by construction, the solution is physically acceptable for the case in which E(r) = 0, there is no guarantee that the new solution with electric field will be physically acceptable and this is what makes it a difficult task to realize.…”

“…Inside of the proposals that take into account the presence of the charge we have different approaches, which can be categorized in two cases, (a) generalizations starting from chargeless solutions to a case in which there is a charge, which are models for which in the absence of charge the chargeless case is recovered and (b) charged models that are not reduced to a chargeless case. Inside of the first class, there have been presented a variety of generalizations from the models of chargeless perfect fluid to the case of a charged perfect fluid, as are the interior solutions of Tolman IV [24,25], Tolman VI, [24,26,27], Tolman VII [24,28,29], Wyman-Adler [30][31][32][33], Buchdahl [34,35], Kuchowicz [36,37], Heintzmann [38,39], Durgapal (n = 4) [40,41], Durgapal (n = 5) [40,42], Vaidya-Tikekar [43][44][45][46], Durgapal-Fuloria [47,48], Knutsen [49,50], Pant [51][52][53], Estevez-Delgado [54,55] among others [13,[56][57][58][59][60]. In the first works, this reduction of a charged model to a chargeless model was an imposed requirement in the construction of charged interior solutions, however, rec...…”

On quintessence star model and strange star

“…To determine the orders of magnitude and see if these are consistent with what we expect for strange quark stars we take the data of the star Her X-1 being a candidate to be strange quark star [66] to obtain its associated values. We know that its mass is M = 0.87M and its radius R = 7.866km, replacing this in (32) we obtain (ν = 0.51192), and replacing this value in Eq. (31) and since σ = k R 2 B g we determine the value of B g to be B g = 97.00476509 Mev fm 3 .…”

“…On the other hand there have been some approaches at a stellar level to describe compact objects [20][21][22][23], considering that the interior of the stars is formed by ordinary neutral matter [24][25][26][27][28][29][30], ordinary charged matter [31][32][33][34][35][36][37], and also by sources which are a combination of ordinary matter and quintessence dark energy, consistent with neutron stars [38]. Neutron or quark stars are not exclusively composed of neutrons or quarks, respectively, but rather these stars are formed predominantly by one of those particles.…”

An interior solution with perfect fluid

“…On the other hand, the stability of the solutions is guaranteed due to the fact that their adiabatic index is a monotonic increasing function with a minimum value γ ≥ 14.615. This exact internal solution can be generalized to the charged or anisotropic case that is able to represent stars with similar characteristics to the ones presented here, with the advantage that the interval of the compactness rate will be greater than in the case of the perfect fluid,[35][36][37] like other solutions with perfect fluid have been generalized [38][39][40][41][42]. Another relevant point is that the solution may be used as2050141-13 Mod.…”