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Hot Jupiters (HJs) are usually defined as giant Jovian-size planets withorbital periods $P \le 10$ days. Although they lie close to the star, severalhave finite eccentricities and significant misalignment angle with respect tothe stellar equator.  Two mechanisms have been proposed to explain the excited and misalignedsub-population of HJs: Lidov-Kozai migration and planet-planet scattering.Although both are based on completely different dynamical phenomena, theyappear to be equally effective in generating hot planets. Nevertheless, therehas been no detailed analysis comparing the predictions of both mechanisms.  In this paper we present numerical simulations of Lidov-Kozai trapping ofsingle planets in compact binary systems. Both the planet and the binary areinitially placed in coplanar orbits, although the inclination of the impactoris assumed random. After the passage of the third star, we follow the orbitaland spin evolution of the planet using analytical models based on the octupoleexpansion of the secular Hamiltonian.  The present work aims at the comparison of the two mechanisms, as anexplanation for the excited and inclined HJs in binary systems. We compare theresults obtained through this paper with results in Beaug\'e & Nesvorn\'y 2012,where the authors analyze how the planet-planet scattering mechanisms works.  Several of the orbital characteristics of the simulated HJs are caused bytidal trapping from quasi-parabolic orbits, independent of the drivingmechanism. These include both the 3-day pile-up and the distribution in theeccentricity vs semimajor axis plane. However, the distribution of theinclinations shows significant differences. While Lidov-Kozai trapping favors amore random distribution, planet-planet scattering shows a large portion ofbodies nearly aligned with the equator of the central star.

Stellar Scattering and the Formation of Hot-Jupiters in Binary Systems