Orbital tori for non-axisymmetric galaxies
  Our Galaxy's bar makes the Galaxy's potential distinctly non-axisymmetric.
All orbits are affected by non-axisymmetry, and significant numbers are
qualitatively changed by being trapped at a resonance with the bar. Orbital
tori are used to compute these effects. Thick-disc orbits are no less likely to
be trapped by corotation or a Lindblad resonance than thin-disc orbits.
Perturbation theory is used to create non-axisymmetric orbital tori from
standard axisymmetric tori, and both trapped and untrapped orbits are recovered
to surprising accuracy. Code is added to the TorusModeller library that makes
it as easy to manipulate non-axisymmetric tori as axisymmetric ones. The
augmented TorusModeller is used to compute the velocity structure of the solar
neighbourhood for bars of different pattern speeds and a simple action-based
distribution function. The technique developed here can be applied to any
non-axisymmetric potential that is stationary in a rotating from - hence also
to classical spiral structure.
