Optical Observations of SS 433 During Eclipses:
Structure of the Accretion Disk

V. P. Goranskii*, S. N. Fabrika**, V. Yu. Rakhimov***, A. A. Panferov**,
A. N. Belov**, and L. V. Bychkova**

*Sternberg Astronomical Institute, Universitetskii pr. 13, Moscow, 119899 Russia

**Special Astrophysical Observatory, Russian Academy of Sciences, Nizhnii Arkhuz, Stavropolskii Krai, 357147 Russia

***Institute of Astrophysics, Academy of Sciences of Tadzhikistan, ul. Bukhogo 22, Dushanbe, 734670 Tadzhikistan

Received August 30, 1996

Abstract—The results of photometric UBVRI, H, and spectral observations of SS 433 during eclipses of the accretion disk are presented. The HeII emission originates near the accretion disk, and has two components—a narrow, nearly Gaussian profile with width FWHM 1000 km/s and a broad two-peaked profile. The regions where the narrow HeII component and H line are emitted experience partial eclipses at orbital 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 HeII line is completely eclipsed at phase 0.0. The blue and red wing components of this line are probably formed in gaseous cocoons around the bases of the relativistic jets. The gas flow velocity in the cocoons is equal 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 region with size 0.20 lies inside this cocoon. The HeII region outside the outwardly propagating jets is not shadowed by the accretion disk, but experiences total eclipses by the optical star of the system.

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