  We present our second paper describing multi-wave-band, time-resolved
spectroscopy of WZ Sge. We analyze the evolution of both optical and IR
emission lines throughout the orbital period and find evidence, in the Balmer
lines, for an optically thin accretion disk and an optically thick hot-spot.
Optical and IR emission lines are used to compute radial velocity curves. Fits
to our radial velocity measurements give an internally inconsistent set of
values for K1, gamma, and the phase of red-to-blue crossing. We present a
probable explanation for these discrepancies and provide evidence for similar
behaviour in other short orbital period dwarf-novae. Selected optical and IR
spectra are measured to determine the accretion disk radii. Values for the disk
radii are found to be strongly dependent on the assumed WD mass and binary
orbital inclination. However, the separation of the peaks in the optical
emission line (i.e. an indication of the outer disk radius) has been found to
be constant during all phases of the super-cycle period over the last 40 years.
