  Most of the planetary systems discovered around binary stars are located at
approximately three semi-major axes from the barycentre of their system,
curiously close to low-order mean-motion resonances (MMRs). The formation
mechanism of these circumbinary planets is not yet fully understood. In situ
formation is extremely challenging because of the strong interaction with the
binary. One possible explanation is that, after their formation, the
interactions between these planets and the surrounding protoplanetary disc
cause them to migrate at velocities dependent on the nature of the disc and the
mass of the exoplanet. Although extensive data can be obtained with direct
hydrodynamical simulations, their computational cost remains too high. On the
other hand, the direct n-body simulations approach allows us to model a large
variety of parameters at much lower cost. We analyse the planetary migration
around a wide variety of binary stars using Stokes-like forces that mimic
planetary migration at a constant rate. Our goal is to identify the main
parameters responsible for the ejection of planets at different resonances with
the inner binary. We performed 4200 n-body simulations with Stokes-like forces
and analysed their evolution and outcome as a function of the properties of
each system. For each simulated exoplanet, we applied an ensemble learning
method for classification in order to clarify the relationship between the
inspected parameters and the process of MMR capture. We identify the capture
probability for different N/1 MMRs, 4/1 being the most prone to capture
exoplanets, with 37% probability, followed by MMR 5/1 with $\sim$ 23% of
probability. The eccentricity of the binary is found to be the most important
parameter in determining the MMR capture of each circumbinary exoplanet,
followed by the mass ratio of the binary and the initial eccentricity of the
planet.
