Can you imagine a Jupiter-like giant planet orbiting its host star with a distance 10 times smaller than the Sun-Mercury distance? Such "hot Jupiters" do exist, and hundreds of them have been observed. But how do they get to their current orbits? One potential formation channel is known as the "high-eccentricity tidal migration". My studies try to understand the details of tidal dissipation in this process from first-principle calculations.