Abstract
This manuscript is related to the construction of relativistic core-envelope model for spherically symmetric charged anisotropic compact objects. The polytropic equation of state is considered for core, while it is linear in the case of envelope. We present that core, envelope and the Reissner Nordstrddot{o}m exterior regions of stars match smoothly. It has been verified that all physical parameters are well behaved in the core and envelope region for the compact stars SAX J1808.4-3658 and 4U1608-52. Various physical parameters inside star are discussed herein, non-singularity and continuity at the junction has been catered as well. Impact of charged compact object together with core-envelope model on the mass, radius and compactification factor is described by graphical representation in both core and envelop regions. The stability of the model is worked out with the help of Tolman–Oppenheimer–Volkoff equations and radial sound speed.
Highlights
Einstein’s general theory of relativity is based on the study of spacetime curvature
It is believed that consideration of spherical symmetry is essential for many solutions of Einstein’s field equations
Symmetric relativistic compact star models were constructed in to analyze the phenomenon of gravitational collapse of stars [8,9]
Summary
Einstein’s general theory of relativity is based on the study of spacetime curvature. Takisa et al [10] described that in spherically symmetric compact stars the physical parameters like density, pressure, temperature and redshift are positive throughout the region. Lakshmi [17] presented model of Einstein’s field equation of anisotropic compact star by using line element with spherically symmetric coordinates and discussed density distribution in anisotropic fluid sphere. Takisa et al [27] discussed the envelope matter and construct anisotropic compact star model. Bonnor [32] presented the model of anisotropic sphere, in his study electrical repulsion affects self-gravitating charged matter. All the properties and conditions of a strong gravitational system as compact star can’t be explained just by a single EoS so we use various EoS’s It can be of the form of linear, polytropic, quadratic or of other dependence. In last section the results are summarized, followed by the list of references
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