  Most exoplanetary systems in binary stars are of S--type, and consist of one
or more planets orbiting a primary star with a wide binary stellar companion.
Gravitational forcing of a single planet by a sufficiently inclined binary
orbit can induce large amplitude oscillations of the planet's eccentricity and
inclination through the Kozai-Lidov (KL) instability. KL cycling was invoked to
explain: the large eccentricities of planetary orbits; the family of close--in
hot Jupiters; and the retrograde planetary orbits in eccentric binary systems.
However, several kinds of perturbations can quench the KL instability, by
inducing fast periapse precessions which stabilize circular orbits of all
inclinations: these could be a Jupiter--mass planet, a massive remnant disc or
general relativistic precession. Indeed, mutual gravitational perturbations in
multiplanet S--type systems can be strong enough to lend a certain dynamical
rigidity to their orbital planes. Here we present a new and faster process that
is driven by this very agent inhibiting KL cycling. Planetary perturbations
enable secular oscillations of planetary eccentricities and inclinations, also
called Laplace--Lagrange (LL) eigenmodes. Interactions with a remnant disc of
planetesimals can make planets migrate, causing a drift of LL mode periods
which can bring one or more LL modes into resonance with binary orbital motion.
The results can be dramatic, ranging from excitation of large eccentricities
and mutual inclinations to total disruption. Not requiring special physical or
initial conditions, binary resonant driving is generic and could have
profoundly altered the architecture of many S--type multiplanet systems. It can
also weaken the multiplanet occurrence rate in wide binaries, and affect planet
formation in close binaries.
