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\subsection{Clump stars}  The work of \citet{Mosser:2012} reveals that the cores of stars in the mass range 1.2...1.5$\mso$ spin down ascending the early RGB as $\approx R^{0.7\pm0.3}$. As stars keep climbing the RGB we expect departures from this law. As the degenerate He core grows in mass, its angular momentum content is determined by the rate of angular momentum transport and by the specific angular momentum of the advected material. Both quantities can in principle change as the star evolves on the RGB: this is because the angular momentum transport mechanism are a function of, fore example, e.g.,  the rate of shear between the core and the envelope, which tend to increase as the star expand. Moreover Even if the torque was a constant,  the amount of specific angular momentum advected in the core decreases rapidly as the core engulfs material that was in the outer convective region. This occurs after the luminosity bump, which is created when the H-burning shell crosses the compositional gradient left by the first dredge up. In our calculations this occur at when  the star has a radius of about XX, corresponding to a value of the large separation of about YY. So it is expected that the rate of spindown should decrease further past the luminosity bump for red giants and depart from the relation $\approx R^{0.7\pm0.3}$ observed by \citet{Mosser:2012}.  This last t (which decreases as the envelope .