Properties of interacting quark star in light of Rastall gravity

Abstract This study explores the properties of quark stars (QSs) formulated with an interacting quark matter equation of state within the framework of Rastall gravity, a modified theory of gravity. We derive the mass-radius relationships and calculate the maximum gravitational masses and their corresponding radii, comparing these results under both Rastall gravity and general relativity. Our analysis incorporates recent observational data, including the GW190425 event, to constrain the model parameters ( <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mrow> <mml:mrow> <mml:mover> <mml:mi>λ</mml:mi> <mml:mo stretchy="false">¯</mml:mo> </mml:mover> </mml:mrow> <mml:mo>,</mml:mo> <mml:mi>η</mml:mi> <mml:mo>,</mml:mo> <mml:msub> <mml:mi>B</mml:mi> <mml:mtext>eff</mml:mtext> </mml:msub> </mml:mrow> </mml:math> ). We also assess the stability of these QSs by evaluating their static stability, adiabatic index, and sound velocity profiles, thus confirming their viability within the modified gravitational framework.

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