Evolution of the radius in uniformly rotating models of the indicated initial masses when adding matter with j_a = 2 × 10¹⁷ cm²s^-1 at a rate of Ṁ = 10^-6M_⊙ yr^-1. The markers indicate every 10% in Ω/Ω_c with the last marker indicating Ω = Ω_c. Prior to mass addition the stars have a small outer convective region, which is more massive in less massive stars. The disappearance of this region is followed by a rapid expansion phase, after which the stars are closer to critical rotation. The line corresponding to the M = 0.675 M_⊙ case is the same as the upper envelope in Fig. 2.