Narrow Results

We discuss the existence of compact stars in the context of $f(R)=R+\alpha R^2+\beta R^{2}ln(\beta R)$ gravity model, where additional logarithmic corrections are assumed. Here, $R$ is the Ricci scalar and $\alpha$, $\beta$ are constant values. Further, the compact stars are considered to be anisotropic in nature, due to the spherical symmetry and high density. For this purpose, we derive the Einstein field equations by considering Krori–Barua spacetime. For our proposed model, the physical acceptability is verified by employing several physical tests like the energy conditions, Herrera cracking concept and stability condition. In addition to this, we also discuss some important properties such as mass–radius relation, surface redshift and the speed of sound are analyzed. Our results are compared with observational stellar mass data, namely, 4U 1820-30, Cen X-3, EXO 1785-248 and LMC X-4. The graphical representation of obtained solutions provide strong evidences for more realistic and viable stellar model.

We consider $R^2$ corrected model, i.e. $f(R)=R+\alpha R^2+\beta R^{2}ln(\beta R)$, where $R$ is the Ricci scalar and $\alpha$, $\beta$ are arbitrary constant values, to investigate some of the interior configurations of static anisotropic spherical charged stellar structures. The existence of electric charge and a strong electric field confirms due to the higher values of pressure distribution and energy density of the matter inside the stars. Furthermore, for compact star configurations, we also consider the simplified MIT bag model equation of state (EoS) given by $p_r=\frac{1}{3}(\rho -4B)$, where $p_r$ is radial pressure, $\rho$ is energy density and $B$ is bag constant. This approach allows to find electric charge from the Einstein–Maxwell field equations. We have extensively discussed the behavior of the electric charge and anisotropic fluid distribution factor for five different values of $\beta$. Interestingly, it is noticed during this study, for smaller values of $\beta$ we get intensity in electric charge. The Tolman–Oppenheimer–Volkoff equation (TOV), is modified in order to carry electric charge. In particular, we model the compact star candidates SAXJ 1808.4–3658 and Vela X-1 and give graphical representation of some important properties such as equilibrium condition, mass-radius ratio and surface redshift. In the end, our calculated solutions provide strong evidences for more realistic and viable charged stellar model.