﹩{\mathrm{log}}_{10}({{\rm{\nabla }}}_{{\rm{s}}})﹩ as a function of log₁₀ (ρ), for 0.3 M_⊙, (a) 10 Myr or (b) 1 Gyr stellar models at ﹩{\rm{\Omega }}=0\mbox{--}20\,{{\rm{\Omega }}}_{\odot }﹩ (Δ5 Ω_⊙). As Ω increases, ∇_s increases throughout the bulk of the stellar interior (Ro ≪ 1), but becomes comparable to the unperturbed model in the near-surface layers (Ro ≫ 1).