deletions | additions       diff --git a/Clump.tex b/Clump.tex  index 3869584..a7914f0 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 sample of stars from Mosser et al., containing objects between 1.2 about 1.2$\mso$  and 1.5$\mso$, revealed that stellar cores seems to slow down considerably during the transition from RGB to core He-burning. They claim this is at odds with the extrapolation of the coupling observed on the lower RGB and simple angular momentum conservation, requiring some different angular momentum transport mechanism at or around the tip of the RGB. We show here that this is not the case and that the observed rotation rate of He-burning stars can be indeed be explained by assuming angular momentum conservation and the fact that the mass of the stellar core increases from the lower RGB to the clump. The size of the He core on the lower RGB is determined by the size of the convective core during the star's main sequence. In the models this can vary between approximatively 0.1 and 0.3$\mso$ for the stars in the mass range of Mosser et al., depending on their mass and the treatment of mixing at the convective boundary. He ignition in the degenerate core occurs when the core mass is $M_{\rm{C}}\approx0.45\mso$,