  Stars in short-period binaries typically have spins that are aligned and
synchronized with the orbit of their companion. In triple systems, however, the
combination of spin and orbital precession can cause the star's rotation to
evolve to a highly misaligned and sub-synchronous equilibrium known as a
Cassini state. We identify a population of recently discovered stars that
exhibit these characteristics and which are already known to have tertiary
companions. These third bodies have a suitable orbital period to allow the
inner binary to evolve into the sub-synchronous Cassini state, which we confirm
with orbital evolution models. We also compute the expected stellar obliquity
and spin period, showing that the observed rotation rates are often slower than
expected from equilibrium tidal models. However, we show that tidal dissipation
via inertial waves can alter the expected spin-orbit misalignment angle and
rotation rate, potentially creating the very slow rotation rates in some
systems. Finally, we show how additional discoveries of such systems can be
used to constrain the tidal physics and orbital evolution histories of stellar
systems.
