Abstract

We study the steady-state orbital distributions of giant planetsmigrating through the combination of theKozai-Lidov (KL) mechanism due to a stellar companion and friction due to tides raised on the planet by the host star. We run a large set of Monte Carlo simulations that describe the secular evolution of a star-planet-star triple system including the effects from general relativistic precession, stellar and planetary spin evolution, and tides. Our simulations show that KL migration produces Hot Jupiters (HJs) with semi-major axes that are generally smaller than in the observations and they can only explain the observations if the following are both true: (1) tidal dissipation at high eccentricities is at least similar to 150 times more efficient than the upper limit inferred from the Jupiter-Io interaction; (2) highly eccentric planets get tidally disrupted at distances greater than or similar to 0.015AU. Based on the occurrence rate and semi-major axis distribution of HJs, we find that KL migration in stellar binaries can produce at most similar to 20% of the observed HJs. Almost no intermediate-period (semi-major axis similar to 0.1 -2AU) planets are formed by this mechanism-migrating planets spend most of their lifetimes undergoing KL oscillations at large orbital separations (> 2AU) or as HJs.