The structural and nucleosynthetic evolution of 3 , 4 , 5 , 6 and 7 M _ { \sun } stars with two metallicities ( Z = 0.005 and 0.02 ) has been computed in detail , from the early pre-main sequence phase up to the thermally pulsing ( TP ) AGB phase or the onset of off-center carbon burning .
Typically 10 to 20 thermal pulses have been followed for each TP-AGB object .
This homogeneous and quite large set of models allows us to present an overview of the thermal pulse properties as well as of the nucleosynthesis accompanying the TP-AGB phase of intermediate-mass stars .

More specifically , after a brief description of the previous evolutionary stages , predictions are given for the isotopic ratios involving C , N , O , Ne , Mg , Al and Si .
Also the surface abundances of { } ^ { 7 } \kern - 0.8 ptLi , { } ^ { 19 } \kern - 0.8 ptF and { } ^ { 23 } \kern - 0.8 ptNa are reported .
As the asymptotic phase of the thermal pulses has been reached for each star , we also indicate how these abundances will probably evolve until the stars completely loose their envelope , by including the evolution of the nucleosynthesis itself .

This article , in its paper form , has been shortened at a level of roughly 60 % as required by directives coming from the A & A editors .
The complete article ( 50 pages containing 37 figures ) is only available in electronic form .