been done by, e.g., @FIH90, but until now these results have not been supported by independent investigations[^1]. In the present work we present a reanalysis of the evolution during the He-flash phase, covering a larger parameter space with respect to the work by Fujimoto and coworkers.

The main characteristics of the evolutionary code used in the present investigation are discussed in the next section; special emphasis is laid upon the numerical algorithms adopted to follow the evolution during the He-flash, and the most relevant differences with respect to previous investigations are indicated. In § \[HeMix\] the evolution through the He core flash in some selected models is presented together with a discussion of the dependence of the subsequent evolution on the , like stellar mass and chemical composition. In the same section, we discuss the change in the surface chemical abundances caused by the appearance of a H shell flash like the one investigated by @FIH90. In § \[PostHe\] we extend the computations for some selected models, which experience a H shell flash, to the following evolutionary phases; we discuss the evolution all along the He-core and -shell burning phase, and compare our results with those corresponding to He-burning models 