  The structure and evolution of central stars of planetary nebulae (CSPNe) is
reviewed. CSPNe represent the rapid transitional stage between the Asymptotic
Giant Branch (AGB) and the white-dwarf domain. It is shown that the whole
evolution off the AGB through the central-star regime depends on the
evolutionary history. The detailed evolution into a white dwarf is controlled
by the internal stellar structure which, in turn, is determined by the duration
of the preceding AGB evolution and therefore by the AGB mass-loss history.
  The evolution of hydrogen-deficient central stars has been a matter of debate
since many years. Convective overshoot appears to be a key ingredient to model
these objects. Various thermal-pulse scenarios with inclusion of overshoot are
discussed, leading to surface abundances in general agreement with those
observed for Wolf-Rayet central stars.
