  KIC 9406652, one of the recently identified IW And-type dwarf novae, is the
best target for studying the tilted disk in cataclysmic variable stars. In a
previous paper by Kimura, Osaki, and Kato (2020), we analyzed its Kepler light
curves and found that its orbital light curves during the brightening stage
were dominated by the reflection effect of the secondary star and varied with
the orientation of the tilted disk; the amplitude was maximized at the minimum
of the super-orbital signal and the phase of the light maximum shifted to an
earlier one with the advance of the super-orbital phase. We argued there that
this was the direct evidence of the retrogradely precessing tilted disk as the
secondary star acts like a reflecting object. In order to confirm this
interpretation, we have performed numerical modeling of orbital light curves in
this paper. We have succeeded in reproducing the main characteristics of the
observed orbital light curves by a simple model in which the secondary star is
irradiated by the tilted disk. We have also constrained the inclination angle,
$i$, of the binary system and the tilt angle, $\theta$, of the disk purely from
photometric considerations. The best-fitting parameter set is found to be $i
\sim$45~deg and $\theta \sim$2.0~deg, respectively. The orbital inclination
thus estimated is consistent with that obtained from the spectroscopic
considerations within the uncertainty limit. On the other hand, the tilt angle
of the disk could be underestimated by using only the semi-amplitude of
super-orbital signals.
