  High-eccentricity migration is an important channel for the formation of hot
Jupiters (HJs). In particular, Lidov-Kozai (LK) oscillations of orbital
eccentricity/inclination induced by a distant planetary or stellar companion,
combined with tidal friction, have been shown to produce HJs on Gyr timescales,
provided that efficient tidal dissipation operates in the planet. We re-examine
this scenario with the inclusion of dynamical tides. When the planet's orbit is
in a high-eccentricity phase, the tidal force from the star excites oscillatory
f-modes and r-modes in the planet. For sufficiently large eccentricity and
small pericentre distance, the mode can grow chaotically over multiple
pericentre passages and eventually dissipate non-linearly, drawing energy from
the orbit and rapidly shrinking the semi-major axis. We study the effect of
such chaotic tides on the planet's orbital evolution. We find that this pathway
produces very eccentric ($e\gtrsim 0.9$) warm Jupiters (WJs) on short
timescales (a few to 100 Myrs). These WJs efficiently circularize to become HJs
due to their persistently small pericentre distances. Chaotic tides can also
save some planets from tidal disruption by truncating the LK eccentricity
oscillations, significantly increasing the HJ formation fraction for a range of
planet masses and radii. Using a population synthesis calculation, we determine
the characteristics of WJs and HJs produced in this scenario, including the
final period distribution, orbital inclinations and stellar obliquities.
Chaotic tides endow LK migration with several favorable features to explain
observations of HJs. We expect that chaotic tides are also important in other
flavours of high-$e$ migration.
