Top: distribution of radii between confirmed planets in the vicinity of the 2:1 (blue) and 3:2 (red) MMR. Dashed line corresponds to equal-size bodies (R₁ = R₂). Middle: radius as a function of the orbital period. Light gray circles indicate the values of planets outside both resonances. Bottom: planetary mass m_i vs. radius R_i for all planets (bodies larger than Jupiter shown in gray). Dashed orange line corresponds to the so-called R^2.06-law by Lissauer et al. (2011), while the fit proposed by Weiss & Marcy (2014) is shown as a continuous orange line. Our own fit, which is calculated for all planets smaller than Jupiter, is presented as a thick green line. Values within 1σ_dis dispersion are contained within the light green region.