  We carry out a comprehensive kinematic and morphological study of the
asymmetrical planetary nebula: NGC 6210, known as the Turtle. The nebula's
spectacularly chaotic appearance has led to proposals that it was shaped by
mass transfer in a triple star system. We study the three-dimensional structure
and kinematics of its shells, lobes, knots, and haloes by combining radial
velocity mapping from multiple long-slit spectra with proper motion
measurements from multi-epoch imaging. We find that the nebula has five
distinct ejection axes. The first is the axis of the bipolar, wind-blown inner
shell, while the second is the axis of the lop-sided, elliptical, fainter, but
more massive intermediate shell. A further two axes are bipolar flows that form
the point symmetric, high-ionization outer lobes, all with inclinations close
to the plane of the sky. The final axis, which is inclined close to the line of
sight, traces collimated outflows of low-ionization knots. We detect major
changes in outflow directions during the planetary nebula phase, starting at or
before the initial ionization of the nebula 3500 years ago. Most notably, the
majority of redshifted low-ionization knots have kinematic ages greater than
2000 years, whereas the majority of blueshifted knots have ages younger than
2000 years. Such a sudden and permanent 180-degree flip in the ejection axis at
a relatively late stage in the nebular evolution is a challenge to models of
planetary nebula formation and shaping.
