Analysis of Balmer Lines Intensities and Radiation Non-Isotropy of SS 433 Jets
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.
KeywordsLine Intensity Accretion Disk Equivalent Width Line Radiation Escape Probability
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