  We place lower limits on the obliquities between debris disks and their host
stars for 31 systems by comparing their disk and stellar inclinations. While
previous studies did not find evidence for misalignment, we identify 6 systems
with minimum obliquities falling between ~30{\deg}-60{\deg}, indicating that
debris disks can be significantly misaligned with their stars. These
high-obliquity systems span a wide range of stellar parameters with spectral
types K through A. Previous works have argued that stars with masses below 1.2
$M_\odot$ (spectral types of ~F6) have magnetic fields strong enough to realign
their rotation axes with the surrounding disk via magnetic warping; given that
we observe high obliquities for relatively low-mass stars, magnetic warping
alone is likely not responsible for the observed misalignment. Yet, chaotic
accretion is expected to result in misalignments of ~20{\deg} at most and
cannot explain the larger obliquities found in this work. While it remains
unclear how primordial misalignment might occur and what role it plays in
determining the spin-orbit alignment of planets, future work expanding this
sample is critical towards understanding the mechanisms that shape these
high-obliquity systems.
