  We present results from new optical and UV spectroscopy of the unusual binary
system SS 433, and we discuss the relationship of the particular spectral
components we observe to the properties of the binary. (1) The continuum
spectrum which we associate with flux from the super-Eddington accretion disk
and the dense part of its wind. (2) H-alpha moving components which are formed
far from the binary orbital plane in the relativistic jets. (3) H-alpha and He
I "stationary" emission lines which we suggest are formed in the disk wind in a
volume larger than the dimensions of the binary. (4) A weak "stationary"
emission feature we identify as a C II 7231,7236 blend that attains maximum
radial velocity at the orbital quadrature of disk recession. (5) Absorption and
emission features from outflowing clumps in the disk wind (seen most clearly in
an episode of blue-shifted Na I emission). (6) We found no clear evidence of
the absorption line spectrum of the optical star, although we point out the
presence of He I absorption features (blended with the stationary emission)
with the expected radial velocity trend at the orbital and precessional phases
when the star might best be seen. (7) A rich interstellar absorption spectrum
of diffuse interstellar bands. The results suggest that the binary is embedded
in an expanding thick disk (detected in recent radio observations) which is fed
by the wind from the super-Eddington accretion disk.
