  Hi'iaka is the larger outer satellite of the dwarf planet Haumea. Using
relative photometry from the Hubble Space Telescope and Magellan and a phase
dispersion minimization analysis, we have identified the rotation period of
Hi'iaka to be ~9.8 hrs (double-peaked). This is ~120 times faster than its
orbital period, creating new questions about the formation of this system and
possible tidal evolution. The rapid rotation suggests that Hi'iaka could have a
significant obliquity and spin precession that could be visible in light curves
within a few years. We then turn to an investigation of what we learn about the
(presently unclear) formation of the Haumea system and family based on this
unexpectedly rapid rotation rate. We explore the importance of the initial
semi-major axis and rotation period in tidal evolution theory and find they
strongly influence the time required to despin to synchronous rotation,
relevant to understanding a wide variety of satellite and binary systems. We
find that despinning tides do not necessarily lead to synchronous spin periods
for Hi'iaka, even if it formed near the Roche limit. Therefore the short
rotation period of Hi'iaka does not rule out significant tidal evolution.
Hi'iaka's spin period is also consistent with formation near its current
location and spin up due to Haumea-centric impactors.
