deletions | additions       diff --git a/Clump.tex b/Clump.tex  index 475e21a..fe58ff9 100644  --- a/Clump.tex  +++ b/Clump.tex 
...
After the red giant branch evolution, stars with $M\lesssim 2\mso$ ignite He in a degenerate core. This leads to a large release of energy, called the He-flash, which during a period of about 2 Myr lifts the degeneracy of the core leading to a stable He-burning phase.   Such transition phase might leave an asteroseismic signature, as suggested by \citet{2012ApJ...744L...6B}.    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 $_{\rm{c}}\approx R^{0.7\pm0.3}$. However extrapolating this law does not explain the slow rotation rate of the clump stars in the sample (P$\sim$30-240 d). This implies that the rate of angular momentum transport increases on the upper RGB RGB,  or that some rapid mixing episode occurs during the He flash. Or both. For example it could be that at the tip of the RGB the 0.45$\mso$ core has some strong differential rotation and that this is erased due to the rapid convective mixing imposed after He ignition. This, together with a slight expansion of the core, would result in a lower rotation rate for the convective core. % the angular momentum content in the layers consituting the 0.45$\mso$ of material in the core mixing due to the appearence of convective rate incre %an increase in the this law to fi seems to show an increase in the rate of angular momentum transport slow down