Fig.1. The spectra of SS433 were obtained with the 6-meter BTA telescope (Russia) and the 8-meter Subaru telescope (Hawaii).
We have taken the spectra nightly twice a day, in Russia, and after 12 hours, in Hawaii. The same spectral region is shown in 8 spectra; two bright lines are seen in each: the line of ionized helium on the right, and the line on the left is the Bowen blend, which consists of 6 lines (3 lines of doubly ionized nitrogen and 3 lines of doubly ionized carbon). All these lines are formed in very hot gas with a temperature of 30-50 thousand degrees. Below the lines, broad contours are shown; these are the discovered super-broad components, one under the helium line, another one under the Bowen blend, and their sum. The numbers in each fragment indicate the orbital phase of the binary system. In the phases 0.92, 0.96, 0.99, 0.03, and 0.07, the supercritical accretion disk is eclipsed to an observer by the donor star. That is why these components are weak.