We study the steady-state orbital distributions of giant planets migrating through the combination of the Kozai-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 : ( i ) tidal dissipation at high eccentricities is at least \sim 150 times more efficient than the upper limit inferred from the Jupiter-Io interaction ; ( ii ) highly eccentric planets get tidally disrupted at distances \gtrsim 0.015 AU . Based on the occurrence rate and semi-major axis distribution of HJs , we find that KL migration in stellar binaries can produce at most \sim 20 \% of the observed HJs . Almost no intermediate-period ( semi-major axis \sim 0.1 - 2 AU ) planets are formed by this mechanism—migrating planets spend most of their lifetimes undergoing KL oscillations at large orbital separations ( > 2 AU ) or as Hot Jupiters .