Distribution of rotation periods, as functions of mass ratio, for non-collision systems with positive total energy. The top and bottom rows correspond to the rotation period of the primary and secondary, at t = 200 days, respectively. The first and second columns show the escape cases, while the third and fourth columns show the unstable cases. The D and S models correspond to models D1–D3 and S1–S3, respectively. The gray crosses are data from Pravec et al. (2019), and only asteroid pairs with q < 0.3 are included in the figure.