Charged anisotropic tolman IV solution in matter-geometry coupled theory

Abstract

Abstract This paper discusses the interior distribution of several anisotropic star models coupled with an electromagnetic field in the context of <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mi>f</mml:mi> <mml:mo stretchy="false">(</mml:mo> <mml:mi mathvariant="italic"></mml:mi> <mml:mo>,</mml:mo> <mml:mi mathvariant="italic"></mml:mi> <mml:mo>,</mml:mo> <mml:mi mathvariant="italic"></mml:mi> <mml:mo stretchy="false">)</mml:mo> </mml:math> gravity, where <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mi mathvariant="italic"></mml:mi> <mml:mo>=</mml:mo> <mml:msub> <mml:mrow> <mml:mi mathvariant="italic"></mml:mi> </mml:mrow> <mml:mrow> <mml:mi>β</mml:mi> <mml:mi>ξ</mml:mi> </mml:mrow> </mml:msub> <mml:msup> <mml:mrow> <mml:mi mathvariant="italic"></mml:mi> </mml:mrow> <mml:mrow> <mml:mi>β</mml:mi> <mml:mi>ξ</mml:mi> </mml:mrow> </mml:msup> </mml:math> . In this regard, a standard model of this modified gravity is taken as <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mi mathvariant="italic"></mml:mi> <mml:mo>+</mml:mo> <mml:msub> <mml:mrow> <mml:mi>ν</mml:mi> </mml:mrow> <mml:mrow> <mml:mn>3</mml:mn> </mml:mrow> </mml:msub> <mml:msub> <mml:mrow> <mml:mi mathvariant="italic"></mml:mi> </mml:mrow> <mml:mrow> <mml:mi>β</mml:mi> <mml:mi>ξ</mml:mi> </mml:mrow> </mml:msub> <mml:msup> <mml:mrow> <mml:mi mathvariant="italic"></mml:mi> </mml:mrow> <mml:mrow> <mml:mi>β</mml:mi> <mml:mi>ξ</mml:mi> </mml:mrow> </mml:msup> </mml:math> , where ν 3 symbolizes an arbitrary coupling constant. We assume a charged spherically symmetric metric that represents the interior geometry of compact quark stars and develop the corresponding modified field equations. These equations are then solved with the help of metric potentials of Tolman IV spacetime and a linear bag model equation of state. We consider the experimental data (i.e. radii and masses) of different quark models such as SMC X-4, SAX J 1808.4-3658, Her X-I and 4U 1820-30 to analyze how the charge and modified corrections affect their physical characteristics. The viability and stability of the resulting model is also checked for the considered star candidates with two different values of ν 3 . We conclude that only two models, Her X-I and 4U 1820-30 show stable behavior in this modified framework for both values of the coupling constant.

Topics & Concepts