See also: https://vixra.org/pdf/1103.0011v3.pdf
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(Wikipedia) SS 433 is a microquasar or eclipsing X-ray binary system, consisting of a stellar-mass black hole accreting matter from an A-type companion star.[5][6] SS 433 is the first discovered microquasar.[7] It is at the centre of the supernova remnant W50.
SS 433's designation comes from the initials of two astronomers at Case Western Reserve University: Nicholas Sanduleak and Charles Bruce Stephenson. It was the 433rd entry in their 1977 catalog of stars with strong emission lines.[7] Its emission lines were studied by Mordehai Milgrom in 1979.[8]
The compact central object is consuming the companion star which rapidly loses mass into an accretion disc formed around the central object. The accretion disc is subject to extreme heating as it spirals into the primary and this heating causes the accretion disc to give off intense X-rays and opposing jets of hot hydrogen along the axis of rotation, above and below the plane of the accretion disc. The material in the jets travels at 26% of the speed of light.[9] The companion star presumably had lower mass than the original primary object and was therefore longer lived. Estimates for its mass range from 3 to 30[10] solar masses. The primary and secondary orbit each other at a very close distance in stellar terms, with an orbital period of 13.082 days. Their orbit is very slightly eccentric, and its period is slowly increasing at a rate of about 1.0×10−7 seconds per second, or about 3 seconds per year.[5]
