  The recent detection of the third planet in Kepler-47 has shown that binary
stars can host several planets in circumbinary orbits. To understand the
evolution of such systems we have performed two-dimensional hydrodynamic
simulations of the circumbinary disc with two embedded planets for several
Kepler systems. In two cases, Kepler-47 and -413, the planets are captured in a
1:1 mean-motion resonance at the planet parking position near the inner edge of
the disc. The orbits are fully aligned, have mean eccentricities of about 0.25
to 0.30, and the planets are entangled in a horseshoe type of motion.
Subsequent n-body simulations without the disc show that the configurations are
stable. Our results point to the existence of a new class of stable resonant
orbits around binary stars. It remains to be seen if such orbits exist in
reality.
