  We study the flux variation in helium white dwarfs (WDs) induced by dynamical
tides for a variety of WD models with effective temperatures ranging from
$T$=10 kK to $T$=26 kK. At linear order, we find the dynamical tide can
significantly perturb the observed flux in hot WDs. If the temperature
$T\gtrsim14$ kK, then the dynamical tide may induce a fractional change in the
flux by >1% when the orbital period is $P_{\rm orb}\simeq 20-60\,{\rm min}$.
The ratio between the flux modulation due to the dynamical tide and that due to
the equilibrium tide (i.e., ellipsoidal variability) increases as the WD's
radius decreases, and it could exceed O(10) if the WD has a radius
$R\lesssim0.03 R_\odot$. Unlike the ellipsoidal variability which is in phase
with the orbital motion, the pulsation caused by the dynamical tide may have a
substantial phase shift. A cold WD with $T\lesssim 10$ kK, on the other hand,
is unlikely to show observable pulsations due to the dynamical tide. At shorter
orbital periods, the dynamical tide may become highly nonlinear. We approximate
this regime by treating the waves as one-way traveling waves and find the flux
variation is typically reduced to 0.1%-1% and the excess phase is likely to be
90 degrees (though with large uncertainty). Even in the traveling-wave limit,
the flux perturbation due to dynamical tide could still exceed the ellipsoidal
variability for compact WDs with $R\lesssim0.02 R_\odot$. We further estimate
the nonlinear flux perturbations oscillating at four times the orbital
frequency dominated by a self-coupled parent g-mode driving low-order daughter
p-modes. The nonlinear flux variation could be nearly 50% of the linear
variation for very hot WD models with $T\gtrsim26$ kK and 1% linear flux
variation. We thus predict both the linear and nonlinear flux variations due to
dynamical tides are likely to have significant observational signatures.
