OPTICAL OBSERVATIONS OF SS-433 DURING ECLIPSES - STRUCTURE OF THE ACCRETION DISK

The results of photometric UBVRI, H-alpha, and spectral observations o f SS 433 during eclipses of the accretion disk are presented. The Hell emission originates near the accretion disk, and has two components-a narrow, nearly Gaussian profile with width FWHM approximate to 1000 k m/s and a broad two-peaked profile. The legions where the narrow HeII component and H-beta line are emitted experience partial eclipses at o rbital phases 0.1 and 0.1-0.2, respectively which indicates that these lines originate in a gaseous flow to the accretion disk. The broad He II line is completely eclipsed at phase 0.0. The blue and red wing com ponents of this line are probably formed in gaseous cocoons around the bases of the relativistic jets. The gas now velocity in the cocoons i s equal to approximate to 1500 km/s. The size of the HeII cocoon is 0. 25-0.30 times the radius of the orbit; an X-ray emitting legion with s ize 0.20 lies inside this cocoon. The HeII region outside the outwardl y propagating jets is not shadowed by the accretion disk, but experien ces total eclipses by the optical star of the system.