  We test the physical model of the relativistic jets in the galactic X-ray
binary SS 433 proposed in our previous paper using additional observations from
the Chandra High Energy Transmission Grating Spectrometer. These observations
sample two new orbital/precessional phase combinations. In the observation near
orbital phase zero, the H- and He-like Fe lines from both receding and
approaching jets are comparably strong and unocculted while the He-like Si line
of the receding jet is significantly weaker than that of the approaching jet.
This condition may imply the cooler parts of the receding jet are eclipsed by
the companion. The X-ray spectrum from this observation has broader emission
lines than obtained in Paper I that may arise from the divergence of a conical
outflow or from Doppler shift variations during the observation. Using recent
optical results, along with the length of the unobscured portion of the
receding jet assuming adiabatic cooling, we calculate the radius of the
companion to be 9.6+/-1.0 R_sun, about one third of the Roche lobe radius. For
a main sequence star, this corresponds to a companion mass of 35+/-7 M_sun,
giving a primary source mass of 20+/-5 M_sun. If our model is correct, this
calculation indicates the compact object is a black hole, and accretion occurs
through a wind process. In a subsequent paper, we will examine the validity of
the adiabatic cooling model of the jets and test the mode of line broadening.
