Top: mode inertia for radial and dipole modes of a 1 M_⊙ RGB star at the bump. The evolution model has been calculated with CESAM (Morel 1997) and the oscillation frequencies were obtained with ADIPLS (Christensen-Dalsgaard 2011). Bottom: normalized integrated rotational kernels of three dipole modes: M₁ and M₂ are g-m modes, whereas M₃ is a p-m mode. The vertical triple-dot-dashed line indicates the mean location of the hydrogen-burning shell, and the vertical dashed line indicates the base of the convective envelope.