  WASP-33b, a hot Jupiter around a hot star, is a rare system in which nodal
precession has been discovered. We updated the model for the nodal precession
of WASP-33b by adding new observational points. Consequently, we found a motion
of the nodal precession spanning 11 years. We present homogenous Doppler
tomographic analyses of eight datasets, including two new datasets from TS23
and HIDES, obtained between 2008 and 2019, to illustrate the variations in the
projected spin-orbit obliquity of WASP-33b and its impact parameter. We also
present its impact parameters based on photometric transit observations
captured by MuSCAT in 2017 and MuSCAT2 in 2018. We derived its real spin-orbit
obliquity $\psi$, stellar spin inclination $i_{s}$, and stellar gravitational
quadrupole moment $J_2$ from the time variation models of the two orbital
parameters. We obtained $\psi = 108.19^{+0.95}_{-0.97}$ deg, $i_s =
58.3^{+4.6}_{-4.2}$ deg, and $J_2=(1.36^{+0.15}_{-0.12}) \times 10^{-4}$. Our
$J_2$ value was slightly smaller than the theoretically predicted value, which
may indicate that its actual stellar internal structure is different from the
theoretical one. We derived the nodal precession speed
$\dot{\theta}=0.507^{+0.025}_{-0.022}$ deg year$^{-1}$, and its period
$P_{\mathrm{pre}}=709^{+33}_{-34}$ years, and found that WASP-33b transits in
front of WASP-33 for only $\sim$ 20 \% of the entire nodal precession period.
