2019MNRAS.483.3465F

Understanding the origin of planets that have formed in binary stars is fundamental to constrain theories of binary and planet formation. The planet occurrence rate in binaries with a separation <=50 au is only ∼one-third that of wider binaries or single stars. This may indicate that a close companion has a ruinous influence on planet formation, because it can truncate the protoplanetary disc and pump up planetesimals eccentricity and collision probability. Nevertheless, observations have revealed a few of these systems, which challenge current planet formation theories. Dynamical interactions can deliver planets into S-type orbits. In this paper, we consider as a possible scenario for forming S-type planets in close binaries the single star-binary star interactions that commonly take place in star clusters. We find that the final fraction and orbital properties of S-type planets in close binaries are mainly determined by the mass ratio of the stars involved in the close encounter, and the initial binary and planet semimajor axes. Present and upcoming missions, such as Transiting Exoplanet Survey Satellite (TESS), Planetary Transits and Oscillations of stars (PLATO), and CHaracterising ExOPlanets Satellite (CHEOPS), may shed new light on the origin of S-type planets in close binaries.