Krori–Barua Bardeen compact stars in <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" altimg="si346.svg" display="inline" id="d1e3478"> <mml:mrow> <mml:mi>f</mml:mi> <mml:mrow> <mml:mo>(</mml:mo> <mml:mi>R</mml:mi> <mml:mo>,</mml:mo> <mml:mi>T</mml:mi> <mml:mo>)</mml:mo> </mml:mrow> </mml:mrow> </mml:math> gravity
Adnan Malik, Zoya Asghar, M. Farasat Shamir
Abstract
The current study emphasizes the impact of electric charge for static spherically symmetric stellar structures using isotropic distribution in f ( R , T ) theory of gravity. For this purpose, we assume the Krori–Barua metric potential, ν ( r ) = B r 2 + C and λ ( r ) = A r 2 , where A , B and C are the unknowns constants. The simplified phenomenological MIT bag equation of state , p = 1 3 ( ρ − 4 B g ) , and a precise form of electrical charge distribution q ( r ) = Q ( r R ) 3 = χ r 3 to be evaluated for the solution of Einstein–Maxwell field equations. To get the value of unknown parameters of the compact structures, we compare the Krori–Barua spacetime to external Bardeen geometry. Moreover, we examine the physical attributes of compact objects by presuming three viable f ( R , T ) models. We analyze the graphical behavior of density and pressure, the Tolman–Oppenheimer–Volkov equation, energy conditions, mass function, surface redshift, and adiabatic index. It is recognized that all the obtained results deliver emphatic evidence for the stability of our considered realistic stars.