  We present observations of SS 433 using the Chandra High Energy Transmission
Grating Spectrometer. Many emission lines of highly ionized elements are
detected with the relativistic blue and red Doppler shifts. The lines are
measurably broadened to 1700 km/s (FWHM) and the widths do not depend
significantly on the characteristic emission temperature, suggesting that the
emission occurs in a freely expanding region of constant collimation with
opening angle of 1.23 +/- 0.06 deg. The blue shifts of lines from low
temperature gas are the same as those of high temperature gas within our
uncertainties, again indicating that the hottest gas we observe to emit
emission lines is already at terminal velocity. Fits to the emission line
fluxes give a range of temperatures in the jet from 5e6 to 1e8 K. We derive the
emission measure as a function of temperature for a four component model that
fits the line flux data. Using the density sensitive Si XIII triplet, the
characteristic electron density is 1e14 cm^{-3}, where the gas temperature is
about 1.3e7 K. Based on an adiabatic expansion model of the jet, the electron
densities drop from ~2e15 to 4e13 cm^{-3} at distances of 2e10 to 2e11 cm from
the apex of the jet cone. The jet mass outflow rate is 1.5e-7 Msun / yr. The
kinetic power is 3.2e38 erg/s, which is x1000 larger than the unabsorbed 2-10
keV X-ray luminosity. The bremsstrahlung emission associated with the lines can
account for the entire continuum; we see no direct evidence for an accretion
disk. The image from zeroth order shows extended emission at a scale of ~2",
aligned in the general direction of the radio jets.
