  In an ongoing effort to explore quantum effects on the interior geometry of
black holes, we explicitly compute the semiclassical flux components
$\left\langle T_{uu}\right\rangle _{ren}$ and $\left\langle T_{vv}\right\rangle
_{ren}$ ($u$ and $v$ being the standard Eddington coordinates) of the
renormalized stress-energy tensor for a minimally-coupled massless quantum
scalar field, in the vicinity of the inner horizon (IH) of a
Reissner-Nordstr\"om black hole. These two flux components seem to dominate the
effect of backreaction in the IH vicinity; and furthermore, their
regularization procedure reveals remarkable simplicity. We consider the
Hartle-Hawking and Unruh quantum states, the latter corresponding to an
evaporating black hole. In both quantum states, we compute $\left\langle
T_{uu}\right\rangle _{ren}$ and $\left\langle T_{vv}\right\rangle _{ren}$ in
the IH vicinity for a wide range of $Q/M$ values. We find that both
$\left\langle T_{uu}\right\rangle _{ren}$ and $\left\langle T_{vv}\right\rangle
_{ren}$ attain finite asymptotic values at the IH. Depending on $Q/M$, these
asymptotic values are found to be either positive or negative (or vanishing
in-between). Note that having a nonvanishing $\left\langle T_{vv}\right\rangle
_{ren}$ at the IH implies the formation of a curvature singularity on its
ingoing section, the Cauchy horizon. Motivated by these findings, we also take
initial steps in the exploration of the backreaction effect of these
semiclassical fluxes on the near-IH geometry.
