Effects of non-minimal matter-geometry coupling on embedding class-one anisotropic solutions
M. Sharif, Tayyab Naseer
Abstract
Abstract This paper investigates some particular anisotropic star models in <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>ω</mml:mi> <mml:mi>α</mml:mi> </mml:mrow> </mml:msub> <mml:msup> <mml:mrow> <mml:mi mathvariant="italic"></mml:mi> </mml:mrow> <mml:mrow> <mml:mi>ω</mml:mi> <mml:mi>α</mml:mi> </mml:mrow> </mml:msup> </mml:math> . We adopt a standard model <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:mo>=</mml:mo> <mml:mi mathvariant="italic"></mml:mi> <mml:mo>+</mml:mo> <mml:mi>ϖ</mml:mi> <mml:mi mathvariant="italic"></mml:mi> </mml:math> , where ϖ indicates a coupling constant. We take spherically symmetric spacetime and develop solutions to the modified field equations corresponding to different choices of the matter Lagrangian by applying ‘embedding class-one’ scheme. For this purpose, we utilize <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mi mathvariant="double-struck">MIT</mml:mi> </mml:math> bag model equation of state and investigate some physical aspects of compact models such as RXJ 1856-37, 4U 1820-30, Cen X-3, SAX J 1808.4-3658 and Her X-I. We use masses and radii of these stars and employ the vanishing radial pressure condition at the boundary to calculate the value of their respective bag constant <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi mathvariant="fraktur">B</mml:mi> </mml:mrow> <mml:mrow> <mml:mi mathvariant="fraktur">c</mml:mi> </mml:mrow> </mml:msub> </mml:math> . Further, we fix ϖ = ± 4 to analyze the behavior of resulting state variables, anisotropy, mass, compactness, surface redshift as well as energy bounds through graphical interpretation for each star model. Two different physical tests are performed to check the stability of the developed solutions. We conclude that ϖ = −4 is more suitable choice for the considered modified model to obtain stable structures of the compact bodies.