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Binary systems are very common among field stars. While this relatively smallnumber of planets in binaries is probably partly due to strong observationalbiases, there is, however, statistical evidence that planets are indeed lessfrequent in binaries with separations smaller than 100 au, strongly suggestingthat the presence of a close in companion star has an adverse effect on planetformation. It is indeed possible for the gravitational pull of the second starto affect all the different stages of planet formation, from proto-planetarydisk formation to dust accumulation into planetesimals, to the accretion ofthese planetesimals into large planetary embryos and, eventually, the finalgrowth of these embryos into planets. For the crucial planetesimal accretionphase, the complex coupling between dynamical perturbations from the binary andfriction due to gas in the protoplanetary disk suggests that planetesimalaccretion might be hampered due to increased, accretion hostile impactvelocities. Likewise, the interplay between the binary secular perturbationsand mean motion resonances lead to unstable regions, where not only planetformation is inhibited, but where a massive body would be ejected from thesystem on a hyperbolic orbit. The amplitude of these two main effects isdifferent for S and P type planets, so that a comparison between the twopopulations might outline the influence of the companion star on the planetformation process. Unfortunately, at present the two populations (circumstellaror circumbinary) are not known equally well and different biases anduncertainties prevent a quantitative comparison. We also highlight the longterm dynamical evolution of both S and P type systems and focus on how thesedifferent evolutions influence the final architecture of planetary systems inbinaries.

Planets in Binaries: Formation and Dynamical Evolution