Compact star models in class I spacetime

Abstract

In the present article, we have presented completely new exact, finite and regular class I solutions of Einstein's field equations i.e. the solutions satisfy the K armarkar condition. For this purpose needfully we have introduced a completely new suitable g rr metric potential to generate the model. We have investigated the various physical aspects for our model such as energy density, pressure, anisotropy, energy conditions, equilibrium, stability, mass, surface and gravitational red-shifts, compactness parameter and their graphical representations. All these physical aspects have ensured that our proposed solutions are wellbehaved and hence represent physically acceptable models for anisotropic fluid spheres. The models have satisfied causality and energy conditions. The presented models are also stable by satisfying Bondi condition and Abreu et al. condition, in equilibrium position and static by satisfying TOV equation, Harrison-Zeldovich-Novikov condition, respectively. For the parameters chosen in the paper are matching in modeling Vela X-1, Cen X-3, EXO 1785-248 and LMC X-4. The M-R graph generated from the solutions is matching the ranges of masses and radii for the considered compact stars. This work also estimated the approximate moment of inertia for the mentioned compact stars.

Charged anisotropic compact objects obeying Karmarkar condition

“…In what follows we shall assume χ = 0, E 2 (r) = 0 and ∆(r) = 0 with the aim to build a toy model representing a compact charged anisotropic fluid sphere. Replacing equations (29)- (30) and (35) into the system (12)- (14) one yields at the following thermodynamic variables…”

All Conformally Flat Einstein--Gauss--Bonnet static Metrics

“…Along these directions, a wide class of astrophysical solutions (including wormholes/compact stars) have been studied ( see, e.g., Refs. [64][65][66][67]). This condition is formulated mathematically via,…”

f(R) wormholes embedded in a pseudo--Euclidean space $E^{5}$

“…Thus, this technology helps to reduce the number of unknowns in order to solve the system of equations. It is remarkably to mention that this techniques has been mainly used in the construction of stellar interiors [41][42][43][44][45][46][47] (and references therein) and also used to obtain wormhole solutions in the GR arena [48][49][50][51]. Additionally, we have assumed the f (R) gravity model given in [52] to obtain the energy-momentum tensor and its components.…”