  Hostile tidal forces may inhibit the formation of Jovian planets in binaries
with semimajor axes of $\la$$50\au$, binaries that might be called ``close'' in
this context. As an alternative to in situ planet formation, a binary can
acquire a giant planet when one of its original members is replaced in a
dynamical interaction with another star that hosts a planet. Simple scaling
relations for the structure and evolution of star clusters, coupled with
analytic arguments regarding binary-single and binary-binary scattering,
indicate that dynamical processes can deposit Jovian planets in $<$1% of close
binaries. If ongoing and future exoplanet surveys measure a much larger
fraction, it may be that giant planets do somehow form frequently in such
systems.
