  This paper discusses the interior distribution of several anisotropic star
models coupled with an electromagnetic field in the context of
$f(\mathcal{R},\mathcal{T},\mathcal{Q})$ gravity, where
$\mathcal{Q}=\mathcal{R}_{\beta\xi}\mathcal{T}^{\beta\xi}$. In this regard, a
standard model of this modified gravity is taken as
$\mathcal{R}+\nu_{3}\mathcal{R}_{\beta\xi}\mathcal{T}^{\beta\xi}$, where
$\nu_{3}$ 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 $\nu_{3}$. 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.
