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 .