THE ORIGIN OF THE X-RAY-EMISSION IN SS-433 IN A HYDRODYNAMICAL MODEL

The possible contribution to the X-ray emission of SS 433 from regions where rapid dense clouds in the relativistic jets interact with rarif ied gas from the accretion disk is examined. The clouds, which move wi th velocities of about 80000 km/s, generate shock waves in the accreti on disk. Behind the shock front, the electrons are heated to temperatu res of about 4 x 10(9) K, and emit photons with energies of more than 300 keV. The high-pressure gas behind the shock front compresses the c louds and generates shock waves in them, whose velocities are of the o rder of several thousand km/s. The gas in the dense clouds passing thr ough the front is rapidly radiatively cooled. Detailed calculations of the radiation spectrum are carried out for front velocities from 2000 to 6000 km/s. Comparison of the calculation results with observations by the GINGA and ASCA satellites sug,nests that the kinetic energy ca rried from the system in the form of these clouds is W < 2 x 1O(39) er g/s. This is close to previous estimates of the bolometric luminosity of the disk, which is consistent with the idea that the accretion in t he SS 433 system is supercritical.