Abstract
In this current study, our main focus is on modeling the specific charged compact star SAX J 1808.4-3658 (M = 0.88 M_{odot }, R = 8.9 km) within the framework of f(R,,T) modified gravity theory using the metric potentials proposed by Tolman–Kuchowicz (Tolman in Phys Rev 55:364, 1939; Kuchowicz in Acta Phys Pol 33:541, 1968) and the interior spacetime is matched to the exterior Reissner–Nordström line element at the surface of the star. Tolman–Kuchowicz metric potentials provide a singularity-free solution which satisfies the stability criteria. Here we have used the simplified phenomenological MIT bag model equation of state (EoS) to solve the Einstein–Maxwell field equations where the density profile (rho ) is related to the radial pressure (p_{mathrm{r}}) as p_{mathrm{r}}(r) = (rho - 4B_{mathrm{g}})/3. Furthermore, to derive the values of the unknown constants a,, b,, B,, C and the bag constant B_{mathrm{g}}, we match our interior spacetime to the exterior Reissner–Nordström line element at the surface of stellar system. In addition, to check the physical validity and stability of our suggested model we evaluate some important properties, such as effective energy density, effective pressures, radial and transverse sound velocities, relativistic adiabatic index, all energy conditions, compactness factor and surface redshift. It is depicted from our current study that all our derived results lie within the physically accepted regime which shows the viability of our present model in the context of f(R,,T) modified gravity.
Highlights
The search for more realistic stellar models within General Relativity (GR) required researchers to connect the macroscopic properties of stars determined through observations to the microphysics
Standard approaches which included assumptions on the metric function, density profiles, pressure profiles, anisotropy parameter and even the matter content which allowed for the system of equations to be integrated gave way to well-motivated techniques intrinsically connected to physics which include an equation of state (EoS), mass profiles linked to surface redshift and compactness of typical stellar structures
In this exposition we have successfully modeled the compact star SAX J 1808.4-3658 within the framework of f (R, T ) modified gravity theory
Summary
The search for more realistic stellar models within GR required researchers to connect the macroscopic properties of stars determined through observations to the microphysics. The model parameters, like density, radial and transverse pressure, anisotropic factor, and electric field, in the background of General Relativity as well as in modified gravity have been successfully obtained. The expression of the anisotropic factor is given in Eq (38), which is defined as the difference between the transverse and radial pressure It may be positive or negative, according as pt > pr or pt < pr, and it is denoted by. We are in a position to check the bound for U given in Eq (57) for different values of γ For this purpose we have to find the numerical values of U from our model which are presented in the following table and it confirms that the inequality is verified for our model of a charged compact star in f (R, T ) gravity. The expression of present in Eq (58) has been given in Eq (38)
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