Analysis of Balmer Lines Intensities and Radiation Non-Isotropy of SS 433 Jets

  • A. A. Panferov
  • S. N. Fabrika
  • L. V. Bychkova
Conference paper
Part of the Astrophysics and Space Science Library book series (ASSL, volume 186)


The relative intensities of Balmer emission lines forming in the relativistic jets of the SS 433 were selected for a long term data of observations. The Balmer decrements are different for the red and blue lets. Using emission line spectrum calculations by Drake and Ulrich (1980) we have found the jets gas clouds have a big enough electron density n e ≈ 1013 cm-3, a normal range of temperatures, T e = (1 − 2) · 104 K and the optical depth in Hα line of 40 – 60. The kinetic luminosity of the jets we obtain is about ≈ 1039 ergs-1. We could understand the observed BDs in terms of two-phase model of emission line cloud in the jet, the cloud consisting of two slabs, foreside hot one with the temperature ≈ 2 · 104 K and back slab with the temperature ≈ 1 · 104 K. The study of the Hα moving lines intensities with the precession phase independently confirms this two-phase model. The front side of the gas cloud is brighter in the Hα line than the back side. The cloud itself radiates in non-isotropic a way in two antiparallel directions, whose axis does not coincide with the jets axis. Such an asymmetry of the jet cloud radiation could be produced by both non-spherical shape of the cloud and shocks in the clouds, rising an escape probability for a line radiation in the direction of a shock.


Line Intensity Accretion Disk Equivalent Width Line Radiation Escape Probability 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.


Unable to display preview. Download preview PDF.

Unable to display preview. Download preview PDF.


  1. Asadullaev, S.S., Cherepashchuk, A.M.: 1986, Soviet Astron. 63, 94Google Scholar
  2. Begelman, M.C., Sarazin, C.L., Hatchett, S.P.: 1980, Astrophys. J. 238, 722ADSCrossRefGoogle Scholar
  3. Borisov, N.V, Fabrika, S.N.: 1987, Soviet Astron. Lett. 13, 200ADSGoogle Scholar
  4. Cherepashchuk, A.M., Aslanov, A.A., Komilov, V.G.: 1982, Soviet Astron. 26, 697ADSGoogle Scholar
  5. Drake, S.A., Ulrich, R.K.: 1980, Astrophys. J. Suppl. Series 42, 351ADSCrossRefGoogle Scholar
  6. Fabrika, S.N., Borisov, N.V.: 1987, Soviet Astron. Lett. 13, 279ADSGoogle Scholar
  7. Kundt, W.: 1985, Astron. Astrophys. 150, 276ADSGoogle Scholar
  8. Luud, L.: 1978, Publications of Tartu observatory, Tartu 46, 55ADSGoogle Scholar
  9. Margon, B.: 1984, Ann. Rev. Astron. Astrophys. 22, 507ADSCrossRefGoogle Scholar
  10. Margon, B., Anderson, S., Aller, L.H., Downes, R.A., Keyes, C.D.: 1984, Astrophys. J. 281, 313ADSCrossRefGoogle Scholar
  11. Panferov, A.A., Fabrika, S.N.: 1992, in preparation Google Scholar
  12. Rakhimov, V.: 1991, private communication Google Scholar
  13. Vittone, A., Rusconi, L., Sedmak, G., Mammano, A., Ciatti, F.: 1983, Astron. Astrophys. Suppl. Series 53, 109ADSGoogle Scholar
  14. Wagner, R.W.: 1986, Astrophys. J. 308, 152ADSCrossRefGoogle Scholar
  15. Wagner, R.W., Newsom, G.H., Foltz, C.B., Byard, P.L.: 1981, Astron. J. 86, 1671ADSCrossRefGoogle Scholar

Copyright information

© Springer Science+Business Media Dordrecht 1993

Authors and Affiliations

  • A. A. Panferov
    • 1
  • S. N. Fabrika
    • 1
  • L. V. Bychkova
    • 1
  1. 1.Special Astrophysical ObservatoryNizhnij ArkhyzRussia

Personalised recommendations