Abstract
We generate a general frame work to solve the Einstein system with an equation of state that describe static spherically symmetric anisotropic matter distribution in terms of a generating function. It is examined for a Van der Waals type equation of state with a physically reasonable form of generating function. The model satisfies all the required major physical properties of a realistic star. It is shown to be stable in the low-density regime that may represent a liquid–gas mixed fluid sphere.
Highlights
Many astrophysical and nuclear physics phenomena are of interest in self-gravitating stellar objects when its structure of matter approaches densities ρ ∼ 0.16 fm−3 at finite temperature (< 20 MeV)
Many exact solutions to the field equations have been generated by different approaches with generalized forms for one of the gravitational potentials that does have an equation of state (EoS) and without [18,19,20,21,22,23,24,25] a particular barotropic EoS relating the pressure to the energy density
Meson condensed states are strongly interacting systems of mesons and baryons whose dynamics is controlled by the underlying chiral symmetry, and quark confinement/deconfinement play an important role in connecting hadron dynamics and quark– gluon dynamics, leading to a unified description
Summary
Many astrophysical and nuclear physics phenomena are of interest in self-gravitating stellar objects when its structure of matter approaches densities ρ ∼ 0.16 fm−3 at finite temperature (< 20 MeV). Many exact solutions to the field equations have been generated by different approaches with generalized forms for one of the gravitational potentials that does have an equation of state (EoS) (linear [2,3,4,5,6,7], quadratic [8,9,10], polytropic [11,12,13,14,15,16], Van der Waals [17], etc.) and without [18,19,20,21,22,23,24,25] a particular barotropic EoS relating the pressure to the energy density.
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