  Solar white-light flares are characterized by an enhancement in the optical
continuum, which are usually large flares (say X- and M-class flares). Here we
report a small C2.3 white-light flare (SOL2022-12-20T04:10) observed by the
\emph{Advanced Space-based Solar Observatory} and the \emph{Chinese H$\alpha$
Solar Explorer}. This flare exhibits an increase of $\approx$6.4\% in the
photospheric Fe \textsc{i} line at 6569.2\,\AA\ and {$\approx$3.2\%} in the
nearby continuum. The continuum at 3600\,\AA\ also shows an enhancement of
$\approx$4.7\%. The white-light brightening kernels are mainly located at the
flare ribbons and co-spatial with nonthermal hard X-ray sources, which implies
that the enhanced white-light emissions are related to nonthermal electron-beam
heating. At the brightening kernels, the Fe \textsc{i} line displays an
absorption profile that has a good Gaussian shape, with a redshift up to
$\approx$1.7 km s$^{-1}$, while the H$\alpha$ line shows an emission profile
though having a central reversal. The H$\alpha$ line profile also shows a red
or blue asymmetry caused by plasma flows with a velocity of several to tens of
km s$^{-1}$. It is interesting to find that the H$\alpha$ asymmetry is opposite
at the conjugate footpoints. It is also found that the CHASE continuum increase
seems to be related to the change of photospheric magnetic field. Our study
provides comprehensive characteristics of a small white-light flare that help
understand the energy release process of white-light flares.
