We investigate the influence of convective overshoot on stellar evolution models of the thermal pulse AGB phase with M _ { \mathrm { ZAMS } } = 3 \mathrm { M } _ { \odot } .
An exponential diffusive overshoot algorithm is applied to all convective boundaries during all evolutionary stages .

We demonstrate that overshooting at the bottom of the pulse-driven convective zone , which forms in the intershell during the He-shell flash , leads to more efficient third dredge-up .
Some overshoot at the bottom of the convective envelope removes the He-H discontinuity , which would otherwise prohibit the occurrence of the third dredge-up for this stellar mass .
However , no correlation between the amount of envelope overshoot and the efficiency of the third dredge-up has been found .

Increasingly efficient third dredge-up eventually leads to a carbon star model .
Due to the partial mixing efficiency in the overshoot region a ^ { 13 } \textrm { C } -pocket can form after the third dredge-up event which may be crucial for n -capture nucleosynthesis .