  The solar ultraviolet intensities of spectral lines originating from Li- and
Na-like ions have been observed to surpass the expectations derived from
plasmas with coronal approximation. The violation of the coronal approximation
can be partially attributed to non-equilibrium ionization (NEI) due to dynamic
processes occurring in the vicinity of the transition region. To investigate
the impact of these dynamics in Alfv\'{e}n-wave-heated coronal loop, a set of
equations governing NEI for multiple ion species was solved numerically in
conjunction with 1.5-dimensional magnetohydrodynamic equations. Following the
injection of Alfv\'{e}n waves from the photosphere, the system undergoes a time
evolution characterized by phases of evaporation, condensation, and
quasi-steady states. During the evaporation phase, the ionization fractions of
Li- and Na-like ions were observed to increase when compared to the fractions
in ionization equilibrium, which lead to the intensity enhancement of up to
1.6. This over-fractionation of Li- and Na-like ions was found to be induced by
the evaporation process. While collisions between shocks and the transition
region temporarily led to deviations from ionization equilibrium, on average
over time, these deviations were negligible. Conversely, under-fractions of the
ionization fraction led to intensity reduction of down to 0.9 during the
condensation phase and the quasi-steady state. Given the dependency of the
over/under-fractionation on mass circulations between the chromosphere and the
corona, these observations will serve as valuable benchmarks to validate not
only Alfv\'{e}n wave models but also other existing mechanisms on coronal
heating.
