  The heating mechanisms of solar white-light flares remain unclear. We present
an X1.0 white-light flare on 2022 October 2 (SOL2022-10-02T20:25) observed by
the Chinese \ha\ Solar Explorer (CHASE) that provides two-dimensional spectra
in the visible light for the full solar disk with a seeing-free condition. The
flare shows a prominent enhancement of $\sim$40\% in the photospheric \fe\ line
at 6569.2 \AA, and the nearby continuum also exhibits a maximum enhancement of
$\sim$40\%. For the continuum near the \fe\ line at 6173 \AA\ from the
Helioseismic and Magnetic Imager (HMI) on board the Solar Dynamics Observatory
(SDO), it is enhanced up to $\sim$20\%. At the white-light kernels, the \fe\
line at 6569.2 \AA\ has a symmetric Gaussian profile that is still in
absorption and the H$\alpha$ line at 6562.8 \AA\ displays a very broad emission
profile with a central reversal plus a red or blue asymmetry. The white-light
kernels are co-spatial with the microwave footpoint sources observed by the
Expanded Owens Valley Solar Array (EOVSA) and the time profile of the
white-light emission matches that of the hard X-ray emission above 30 keV from
the Gamma-ray Burst Monitor (GBM) on Fermi. These facts indicate that the
white-light emission is qualitatively related to a nonthermal electron beam. We
also perform a radiative hydrodynamic simulation with the electron beam
parameters constrained by the hard X-ray observations from Fermi/GBM. The
result reveals that the white-light enhancement cannot be well explained by a
pure electron-beam heating together with its induced radiative backwarming but
may need additional heating sources such as \alfven\ waves.
