  We present the first detailed kinematical analysis of the planetary nebula
Abell 63, which is known to contain the eclipsing close-binary nucleus UU Sge.
Abell 63 provides an important test case in investigating the role of
close-binary central stars on the evolution of planetary nebulae.
  Longslit observations were obtained using the Manchester echelle spectrometer
combined with the 2.1-m San Pedro Martir Telescope. The spectra reveal that the
central bright rim of Abell 63 has a tube-like structure. A deep image shows
collimated lobes extending from the nebula, which are shown to be high-velocity
outflows. The kinematic ages of the nebular rim and the extended lobes are
calculated to be 8400+/-500 years and 12900+/-2800 years, respectively, which
suggests that the lobes were formed at an earlier stage than the nebular rim.
This is consistent with expectations that disk-generated jets form immediately
after the common envelope phase.
  A morphological-kinematical model of the central nebula is presented and the
best-fit model is found to have the same inclination as the orbital plane of
the central binary system; this is the first proof that a close-binary system
directly affects the shaping of its nebula. A Hubble-type flow is
well-established in the morphological-kinematical modelling of the observed
line profiles and imagery.
  Two possible formation models for the elongated lobes of Abell 63 are
considered (1) a low-density, pressure-driven jet excavates a cavity in the
remnant AGB envelope; (2) high-density bullets form the lobes in a single
ballistic ejection event.
