Quintessences compact star with Durgapal potential

Abstract

A compact star model formed by quintessence and ordinary matter is presented, both sources have anisotropic pressures and are described by linear state equations, also the state equation of the tangential pressure for the ordinary matter incorporates the effect of This is an Open Access article published by World Scientific Publishing Company. It is distributed under the terms of the Creative Commons Attribution 4.0 (CC BY) License which permits use, distribution and reproduction in any medium, provided the original work is properly cited.* Corresponding author. 2050144-1 Mod. Phys. Lett. A 2020.35. Downloaded from www.worldscientific.com by 44.224.250.200 on 07/11/20. Re-use and distribution is strictly not permitted, except for Open Access articles. G. Estevez-Delgado et al.the quintessence. It is shown that depending on the compactness of the star u = GM/c 2 R the constant of proportionality µ between the density of the ordinary matter and the radial pressure, Pr = µc 2 (ρ − ρ b ), has an interval of values which is consistent with the possibility that the matter is formed by a mixture of particles like quarks, neutrons and electrons and not only by one type of them. The geometry is described by the Durgapal metric for n = 5 and each one of the pressures and densities is positive, finite and monotonic decreasing, as well as satisfying the condition of causality and of stability v 2 t − v 2 r < 0, which makes our model physically acceptable. The maximum compactness that we have is u ≤ 0.28551, so we can apply our solution considering the observational data of mass and radii M = (2.01 ± 0.04) M ⊙ , R ∈ [12.062, 12.957] km which generate a compactness 0.22448 ≤ u ≤ 0.25448 associated to the star PSR J0348 + 0432. In this case, the interval of µ ∈ [0.78055, 1] and its maximum central density ρc and in the surface ρ b of the star are ρc = 7.0387 × 10 17 kg/m 3 and ρ b = 4.6807 × 10 17 kg/m 3 , respectively, meanwhile the central density of the quintessence ρqc = 3.4792 × 10 16 kg/m 3 .

On quintessence star model and strange star

“…Particularly it is natural to ask the following questions. What type of star represent the perfect fluid models in the context of the model posed in this investigation [67][68][69]? How is the spectrum of solutions modified if we allow ρ q to admit regions where it is negative?…”

Determination of the charge for strange stars

“…In these models part of the difficulty lies in being able to obtain that the union between two or more regions, for example in the case of two regions, one an inner layer we will call core and an outer layer we will call envelope both with distinct pressures, the conditions of continuity are satisfied between the first fundamental form and the second fundamental form, described by the conditions of Israel [28]. As such, the description of their interior is not a simple task and with the intent of obtaining a better description for stars with a greater compactness, taking elements that help us understand these, there have been proposals for state equations that even consider the existence of quintessence inside them [29][30][31][32][33] showing that this model is consistent with the required properties of behaviour and with the observational data of mass and radius. On the other hand, the possibility that quark stars exist arises due to the fact that in the interior of the neutron stars there may be a phase transition from neutrons to hyperons and strange quark matter [34].…”

Wetland degradation of a ramsar site: A study of East Kolkata wetlands of West Bengal, India

“…Murad et al [79] and Maurya et al [80] presented the interior solutions of the Einstein-Maxwell field equations for a static spherically symmetric charged perfect fluid in the framework of general relativity with Durapal metric. Islam et al [81] studied the strange stars in the Durgapal-IV spacetime and the quintessence compact star is also studied in the Durgapal spacetime [82]. Very recently, Rej [83] studied the uncharged isotropic compact stars model in the bigravity with the Durgapal-IV metric, also, Rej et al [84] studied the isotropic Durgapal-IV relativistic fluid sphere in the ground of f (R, T ) gravity.…”