  The X-ray spectrum of the Galactic microquasar SS 433 contains a rich set of
emission lines of highly ionized atoms of heavy elements whose significant
Doppler shift leaves no doubt that they are produced in collimated relativistic
jets of outflowing material. We have performed a systematic analysis of the
high-resolution X-ray spectra obtained by the Chandra observatory to determine
the parameters of the jets within the multitemperature model of their emission
that self-consistently predicts the source's line and continuum spectrum. The
spectrum of SS 433 at energies below 3 keV is shown to be statistically
satisfactorily described by the jet emission model, while the introduction of
an additional hard component is required above 3 keV. We summarize the jet
parameters (bulk velocity, opening angle, kinetic luminosity, base temperature,
and relative elemental abundances) derived by fitting the data below 3 keV and
describe the revealed degeneracies and systematic effects due to the presence
of an additional component. Using the derived parameters, we show that the hard
component is compatible with the emission from the hot (up to 40 keV) extension
of the visible part of the jets moderately absorbed ($N_H \sim 2 \times
10^{23}$ cm$^{-2}$) in the cold-wind material. The combined X-ray emission
model constructed in this way allows the broadband spectrum of SS 433 to be
described self-consistently.
