  We present the first evolutionary models of intermediate mass stars up to
their thermal pulses which include effects of rotation on the stellar structure
as well as rotationally induced mixing of chemical species and angular
momentum. We find a significant angular momentum transport from the core to the
hydrogen-rich envelope and obtain a white dwarf rotation rate comparable to
current observational upper limits of 50 km/s.
  Large angular momentum gradients at the bottom of the convective envelope and
the tip of the pulse driven convective shell are shown to produce marked
chemical mixing between the proton-rich and the 12C-rich layers during the so
called third dredge-up. This leads to a subsequent production of 13C which is
followed by neutron production through 13C(alpha,n) in radiative layers in
between thermal pulses. Although uncertainties in the efficiency of rotational
mixing processes persist, we conclude that rotation is capable of producing a
13C-rich layer as required for the occurrence of the s-process in TP-AGB stars.
