  We study the local dark matter distribution in two models for the Milky Way
(MW)-Large Magellanic Cloud (LMC) interaction. The effect of the LMC on the
local dark matter distribution is dependent on the evolution of the MW-LMC
system, such that a static model is insufficient to accurately model the dark
matter velocity distribution in the solar neighbourhood. An evolved model
boosts local LMC dark matter particle velocities by nearly 50%, to a median
value of $\approx750$km/s. MW dark matter particles also experience a velocity
boost, which we identify as being caused by reflex motion owing to the infall
of the LMC. We study the implications of LMC particles in the solar
neighbourhood for dark matter detection experiments. Specifically, the
directionality of LMC particles is distinguishable from the MW particles, with
a difference in the apparent origin centroid location between the MW and LMC
particles of $26\pm6 ^\circ$. This unique identifier, along with their high
velocities, can be utilised by directional detectors to search for dark matter
particles originating in the LMC.
