Charged stellar structures with Adler–Finch–Skea geometry in Ricci-inverse gravity

Abstract We have developed a class of charged, anisotropic, and spherically symmetric solutions, described by the function <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 class="MJX-tex-calligraphic" mathvariant="script">R</mml:mi> <mml:mo>,</mml:mo> <mml:mi class="MJX-tex-calligraphic" mathvariant="script">A</mml:mi> <mml:mo stretchy="false">)</mml:mo> <mml:mo>=</mml:mo> <mml:mi class="MJX-tex-calligraphic" mathvariant="script">R</mml:mi> <mml:mo>+</mml:mo> <mml:mi>α</mml:mi> <mml:mi class="MJX-tex-calligraphic" mathvariant="script">A</mml:mi> </mml:math> , where <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mi class="MJX-tex-calligraphic" mathvariant="script">R</mml:mi> </mml:math> represents the Ricci scalar, <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mi class="MJX-tex-calligraphic" mathvariant="script">A</mml:mi> </mml:math> is the anticurvature scalar, and α is the coupling constant. The model was constructed using the Karmarkar condition to obtain the radial metric component, while the time metric component followed the approach proposed by Adler. We assumed a specific charge distribution inside the star to build the model. To ensure a smooth spacetime transition, we established boundary conditions, considering Bardeen's solution for the exterior spacetime. Additionally, we examined various physical aspects, such as energy density, pressure components, pressure anisotropy, energy conditions, the equation of state, surface redshift, compactness factor, adiabatic index, sound speed, and the Tolman–Oppenheimer–Volkoff equilibrium condition. All these conditions were met, demonstrating that the solutions we obtained are physically viable.