  The surfaces of many white dwarfs are polluted by metals, implying a recent
accretion event. The tidal disruption of planetesimals is a viable source of
white dwarf pollution and offers a unique window into the composition of
exoplanet systems. The question of how planetary material enters the tidal
disruption radius of the white dwarf is currently unresolved. Using a series of
$N$-body simulations, we explore the response of the surrounding planetesimal
debris disk as the white dwarf receives a natal kick caused by anisotropic mass
loss on the asymptotic giant branch. We find that the kick can form an
apse-aligned, eccentric debris disk in the range 30 to 240 AU which corresponds
to the orbits of Neptune, the Kuiper Belt, and the scattered disk in our solar
system. In addition, many planetesimals beyond 240 AU flip to counter-rotating
orbits. Assuming an isotropic distribution of kicks, we predict that
approximately 80% of white dwarf debris disks should exhibit significant
apsidal alignment and fraction of counter-rotating orbits. The eccentric disk
is able to efficiently and continuously torque planetesimals onto radial,
star-grazing orbits. We show that the kick causes both an initial burst in
tidal disruption events as well as an extended period of 100 Myr where tidal
disruption rates are consistent with observed mass accretion rates on polluted
white dwarfs.
