  Motivated by the LMC's impact on the integral of motion space of the stellar
halo, we run an $N$-body merger simulation to produce a population of halo-like
stars. We subsequently move to a test particle simulation, in which the LMC
perturbs this debris. When an axisymmetric potential is assumed for the final
snapshot of the $N$-body merger remnant, a series of vertical striations in
$(L_z, E)$ space form as the LMC approaches its pericentre. These result from
the formation of overdensities in angular momentum owing to a relationship
between the precession rate of near radial orbits and the torquing of these
orbits by the LMC. This effect is heavily dependent on the shape of the inner
potential. If a quadrupole component of the potential is included these
striations become significantly less apparent due to the difference in
precession rate between the two potentials. The absence of these features in
data, and the dramatic change in orbital plane precession rate, discourages the
use of an axisymmetric potential for highly eccentric orbits accreted from a
massive GSE-like merger. Given the link between appearance of these striations
and the shape of the potential, this effect may provide a new method of
constraining the axisymmetry of the halo.
