Ginga observations of SS433 have been made at various precessional and orbital phases on six occasions from 1987 to 1991. Although some of the results have been published, we have re-analyzed all data systematically in order to understand the X-ray emission mechanism in SS433. All data confirm that the iron K emission in the non-eclipse spectra of SS433 can be resolved into a narrow and a broad line. The apparent equivalent width of the narrow line is estimated to be about 1keV, while that of the broad line is 2keV or more. The centroid energy of the narrow line depends on the precessional phase, according to the Doppler shift expected from the blue jet, while that of the broad line is approximately constant for all precessional phases. The intensity and width of the broad line, however, change according to the precessional phase, being proportional to the X-ray continuum flux, while the intensity of the narrow line in the rest frame of the jet is relatively constant. The variation of X-ray continuum flux cannot be explained by relativistic boosting effect alone. We conclude that the observed variations of the continuum and the broad line depend mainly on the geometrical viewing condition, and are not caused by temporal variability. The possible origin of the broad line is also discussed. Furthermore, an eclipse-like feature of X-rays just after the orbital eclipse is studied in detail in 1990 data, whose spectral properties are similar to those in the X-ray eclipse. The observations of such a `second eclipse' tend to suggest a large opaque structure related to the binary system of SS433.
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