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   PR # 11031
    SS 433 exhibits the X-ray Fe emission line with its energy, profile
    and intensity varying with the precession of the relativistic jets.
    We propose ASCA observations of SS 433 to spectroscopically resolve
    the narrow lines, i.e.direct components from the jet.  In order to
    study the jets from various aspect angles, observations must be care-
    fully sampled over the entire precession and binary phases.  Unfortun
    ately, the 162-day precession period is close to the half-year period
    of the sun-angle window.  Coverage over the entire precession phases
    is possible only with a careful scheduling over the four years.  The
    PV phase observations covered the phase 0.98 - 0.16.  In AO-1, we
    propose to coverphase ~0.3. The coverage at phases 0.5, 0.65, and 0.8
   will be proposed for the subse
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