  We explore the possibility that the observed population of Galactic
hypervelocity stars (HVSs) originate as runaway stars from the Large Magellanic
Cloud (LMC). Pairing a binary evolution code with an N-body simulation of the
interaction of the LMC with the Milky Way, we predict the spatial distribution
and kinematics of an LMC runaway population. We find that runaway stars from
the LMC can contribute Galactic HVSs at a rate of $3 \times
10^{-6}\;\mathrm{yr}^{-1}$. This is composed of stars at different points of
stellar evolution, ranging from the main-sequence to those at the tip of the
asymptotic giant branch. We find that the known B-type HVSs have kinematics
which are consistent with an LMC origin. There is an additional population of
hypervelocity white dwarfs whose progenitors were massive runaway stars.
Runaways which are even more massive will themselves go supernova, producing a
remnant whose velocity will be modulated by a supernova kick. This latter
scenario has some exotic consequences, such as pulsars and supernovae far from
star-forming regions, and a small rate of microlensing from compact sources
around the halo of the LMC.
