  In the context of $f\left(R, T\right) = R + 2 \beta T$ gravity, where $R$ is
the Ricci scalar and $T$ is the trace of the energy-momentum tensor, the
equilibrium structure of charged anisotropic white dwarfs (WDs) is studied. The
stellar equations for the general case are derived and numerical solutions are
found for the Chandrasekhar equation of state (EoS) and a charge density
distribution proportional to the energy density $\rho_{\text{ch}} = \alpha
\rho$. By adjusting different parameters, the properties of the solutions under
various conditions are compared. Most importantly, by going beyond the trivial
WD in GR in various ways, the solutions may exhibit super-Chandrasekhar
behavior. This article is a study of a WD structure, and the results obtained
may have a contrasting effect on astronomical observations such as
superluminous type Ia supernovae.
