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 \pm 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 \pm 7 M _ { \sun } , giving a primary source mass of 20 \pm 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 .