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_{odot }, 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 varGamma , 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., n=0.5, 1.08, 1.66, 2.24, 2.82 and 3.4.
Highlights
On the other hand, a stellar configuration not necessary need to meet the isotropic condition at all
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., n = 0.5, 1.08, 1.66, 2.24, 2.82 and 3.4
In order to guarantee it, the stress–energy tensor needs to comply with the null energy condition (NEC), which infers that local mass–energy density must not be negative, the weak energy condition (WEC) in both radial and tangential direction, suggesting that the flow of energy interior the spherical object must not be quicker than the speed of light
Summary
A stellar configuration not necessary need to meet the isotropic condition at all (equal radial pr and tangential pt pressure). The nearness of anisotropy presents a few highlights in the distribution of matter, e.g. if we have a positive anisotropy parameter Δ ≡ pt − pr > 0, the astrophysical configuration encounters a repulsive force (attractive in the situation of negative anisotropy parameter) that counteracts the gravitational slope It permits the construction of more compact stars when utilizing anisotropic fluid than when utilizing isotropic fluid [27,33,35,82,83]. Our stellar model incorporates a family of new solutions for a static spherically symmetric anisotropic ïnCuid structure within the class I condition to find the full space-time representation interior the stellar system.
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