Evolution of the planet semi-major axis with respect to time for a binary eccentricity of e_B = 0.2 and a 10^-5 au/yr migration velocity. The semi-major axis of the binary has been set to a_B = 0.4 au. The plot illustrates the migration, then ejection, of the planet after it has been trapped into a 1:6 resonance. The effect of the 1:7 resonance, weaker, is also visible on the plot. As the planet has a perturbed Keplerian motion around the binary, the exact locations of MMRs are not straightforward to derive (see Appendix B).