Left: semimajor axis vs. eccentricities of exoplanets in S-type orbits. The circles and stars represent systems with one or multiple planets, respectively. The color bar represents the semimajor axis of the binary star (a_B) for planets with eccentricities greater than 0.8. Shaded regions highlight the hot, warm and cold Jupiter populations. The data are from the Encyclopedia of Exoplanets. Right: orbital stability limits for systems with e ≥ 0.8. The effects of a binary stellar companion with M_B = 0.8 M_⊙ are shown for two eccentricities: e_B = 0.05 (purple) and e_B = 0.9 (yellow). The stars indicate the observed semimajor axis a_B of the binary, while the horizontal lines extend from periapsis q_B = a_B(1 − e_B) to apoapsis Q_B = a_B(1 + e_B). Similarly, the horizontal black circles and lines depict the semimajor axis, peri- and apoapsis of the planet, respectively. The purple and yellow bars extend to the critical semimajor axis a_crit for the planetary orbit, above which it would not be dynamically stable following Holman & Wiegert (1999), for each binary eccentricity. The filled bars indicate that the system is dynamically unstable under the corresponding binary eccentricity, while the open bars indicate stability.