  We start by reviewing our previous work on retrograde orbital configurations
and on modeling and identifying retrograde resonances. Then, we present new
results regarding the enhanced stability of retrograde configurations with
respect to prograde configurations in the low mass ratio regime of the planar
circular restricted 3-body problem. Motivated by the recent discovery of small
bodies which are in retrograde resonance with the Solar System's giant planets
we then explore the case with mass ratio 0.001 and show new stability maps in a
grid of semi-major axis versus eccentricity for the 2/1 and 1/2 retrograde
resonances. Finally, we explain how the stability borders of the 2/1 and 1/2
retrograde resonances are related to the resonant orbits' geometry.
