  Galaxy morphology is one of the most fundamental ways to describe galaxy
properties, but the morphology we observe may be affected by wavelength and
spatial resolution, which may introduce systematic bias when comparing galaxies
at different redshift. Taking advantage of the broad wavelength coverage from
optical to near-IR and high resolution NIRCam instrument of JWST, we measure
the non-parametric morphological parameters of a total of 1376 galaxies at
$z\simeq$0.8-3.0 in the CEERS field through an optimized code called
{\tt\string statmorph\_csst}. We divide our sample into three redshift
intervals and investigate the wavelength- and redshift-dependence of the
morphological parameters. We also explore how the widely-used galaxy type
classification methods based on the morphological parameters depend on
wavelength and spatial resolution. We find that there are variations in all
morphological parameters with rest-frame wavelength ($\lambda_{\rm rf}$),
especially at the short wavelength end, and the $\lambda_{\rm rf}$ mainly
affects the classification between late-type and early-type galaxy. As the
$\lambda_{\rm rf}$ increases, the galaxies on the $G-M_{20}$ diagram move to
the upper left with a slope of -0.23$\pm$0.03 on average. We find that spatial
resolution mainly affects the merger identification. The merger fraction in
F200W resolution can be $\ga$2 times larger than that in F444W resolution.
Furthermore, We compare the morphological parameter evolution of galaxies with
different stellar masses. We find that there are differences in the
morphological evolution of high- and low-mass (log$M_*\geqslant$10 and
9$<$log$M_*<$10) galaxies in the studied redshift range, which may be caused by
their different evolution paths.
