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The equilibrium configuration of white dwarfs composed of a charged perfectfluid are investigated in the context of the $f(R,\mathcal{T})$ gravity, forwhich $R$ and $\mathcal{T}$ stand for the Ricci scalar and the trace of theenergy-momentum tensor, respectively. By considering the functional form $f(R,\mathcal{T})=R+2\chi \mathcal{T}$, where $\chi$ is the matter-geometry couplingconstant, and for a Gaussian ansatz for the electric distribution, somephysical properties of charged white dwarfs were derived, namely: mass, radius,charge, electric field, effective pressure and energy density; their dependenceon the parameter $\chi$ was also derived. In particular, the $\chi$ valueimportant for the equilibrium configurations of charged white dwarfs has thesame scale of $10^{-4}$ of that for non-charged stars and the order of thecharge was $10^{20}$C, which is scales with the value of one solar mass, i.e.,$\sqrt{G}M_\odot\sim 10^{20}$C. We have also shown that charged white dwarfstars in the context of the $f(R,\mathcal{T})$ have surface electric fieldsgenerally below the Schwinger limit of $1.3\times 10^{18}$V/m. In particular, astriking feature of the coupling between the effects of charge and$f(R,\mathcal{T})$ gravity theory is that the modifications in the backgroundgravity increase the stellar radius, which in turn diminishes the surfaceelectric field, thus enhancing stellar stability of charged stars. Mostimportantly, our study reveals that the present $f(R,T)$ gravity model cansuitably explain the super-Chandrasekhar limiting mass white dwarfs, which aresupposed to be the reason behind the over-luminous SNeIa and remain mostlyunexplained in the background of general relativity (GR).

Study of the charged super-Chandrasekhar limiting mass white dwarfs in the $f(R,\mathcal{T})$ gravity