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High-eccentricity migration is an important channel for the formation of hotJupiters (HJs). In particular, Lidov-Kozai (LK) oscillations of orbitaleccentricity/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-examinethis scenario with the inclusion of dynamical tides. When the planet's orbit isin a high-eccentricity phase, the tidal force from the star excites oscillatoryf-modes and r-modes in the planet. For sufficiently large eccentricity andsmall pericentre distance, the mode can grow chaotically over multiplepericentre passages and eventually dissipate non-linearly, drawing energy fromthe orbit and rapidly shrinking the semi-major axis. We study the effect ofsuch chaotic tides on the planet's orbital evolution. We find that this pathwayproduces very eccentric ($e\gtrsim 0.9$) warm Jupiters (WJs) on shorttimescales (a few to 100 Myrs). These WJs efficiently circularize to become HJsdue to their persistently small pericentre distances. Chaotic tides can alsosave some planets from tidal disruption by truncating the LK eccentricityoscillations, significantly increasing the HJ formation fraction for a range ofplanet masses and radii. Using a population synthesis calculation, we determinethe characteristics of WJs and HJs produced in this scenario, including thefinal period distribution, orbital inclinations and stellar obliquities.Chaotic tides endow LK migration with several favorable features to explainobservations of HJs. We expect that chaotic tides are also important in otherflavours of high-$e$ migration.

Chaotic Tides in Migrating Gas Giants: Forming Hot and Transient Warm Jupiters via High-Eccentricity Migration