Anisotropic relativistic fluid spheres: an embedding class I approach

Abstract

In this work, we present a new class of analytic and well-behaved solution to Einstein's field equations describing anisotropic matter distribution. It's achieved in the embedding class one spacetime framework using Karmarkar's condition. We perform our analysis by proposing a new metric potential g rr which yields us a physically viable performance of all physical variables. The obtained model is representing the physical features of the solution in detail, analytically as well as graphically for strange star candidate SAX J1808.4-3658 (Mass = 0.9 M , radius = 7.951 km), with different values of parameter n ranging from 0.5 to 3.4. Our suggested solution is free from physical and geometric singularities, satisfies causality condition, Abreu's criterion and relativistic adiabatic index Γ , and exhibits well-behaved nature, as well as, all energy conditions and equilibrium condition are well-defined, which implies that our model is physically acceptable. The physical sensitivity of the moment of inertia (I) obtained from the solutions is confirmed by the Bejger−Haensel concept, which could provide a precise tool to the matching rigidity of the state equation due to different values of n viz.,

Anisotropic neutron stars modelling: constraints in Krori–Barua spacetime

“…A lot of anisotropic solutions and anisotropic compact star models have been proposed and studied [22][23][24][25][26][27][28][29][30][31][32]. Ivanov has calculated general bounds on the redshift for any anisotropic compact star in Ref.…”

An EGD model in the background of embedding class I space–time

“…This condition provides an extensive tool for solving Einstein's field equations and investigate new relativistic astrophysical compact stellar structures. Recently, several solutions were obtained in the context of charged and anisotropic matter distributions with well defined compact structures for class I space-time [10][11][12][13][14][15][16][17][18][19][20][21][22][23][24][25][26] (and references contained therein).…”

MGD-decoupled black holes, anisotropic fluids and holographic entanglement entropy

“…Refs. [2,3,25,28,49] shows that for positive anisotropy, when p t − p r > 0, the compact stellar configuration repulsive force counterbalances the gravitational pressure. Hence, anisotropic stars are more likely to exist in astrophysics, being also more stable, as discussed in Refs.…”

“…Experimental data shows the existence of such astrophysical objects, observed at very high densi-ties, including X-ray pulsars, bursters and sources [58,59]. Recently, strange stars candidates, illustrated by the astrophysical SAX J1808.4-3658 compact stellar configurations, were described by the anisotropic MGD-decoupling [49]. In addition, anisotropic neutron compact stellar configurations were used to describe the compact objects 4U 1820.30, 4U 1728.34, PSR J0348+0432, RX J185635.3754, PSR 0943+10, the binary pulsar SAX J1808.4-3658 and X-ray binaries Her X-1 and Cen X-3, whose stability was also investigated in the MGD-decoupling context [60,61].…”