SS 433 as an eclipsing binary

INTEGRAL observations of SS433, a supercritically accreting microquasar with hard spectrum

“…This confirmed the evolutionary status of SS433 as a massive X-ray binary at an advanced evolutionary stage (Cherepashchuk 1981(Cherepashchuk , 1988) with supercritical accretion (Shakura & Sunyaev 1973 (Gies et al 2002a) may indicate that the observed large width of X-ray eclipse in SS433 can be due to collision stellar winds of the binary components (Cherepashchuk et al 1995). So it is established now that SS433 is a microquasar with a black hole (BH), supercritical precessing accretion disc and precessing quasi-stationary relativistic jets.…”

“…• , Namiki et al 2003), precessing jets (Margon 1984;Cherepashchuk 1981Cherepashchuk , 1988Crampton & Hutchings 1981). The system exhibits three photometric and spectral periodicities related to precession (P prec = 162. d 5), orbital (P orb = 13.…”

Monte Carlo simulations of the broad-band X-ray continuum of SS433

“…It is one of the brightest stars in the Galaxy, the bolometric luminosity of the object assuming isotropic radiation is L bol ∼ 10 40 erg s −1 (Cherepashchuk, Aslanov & Kornilov 1982). SS433 is a close binary system with an orbital period of 13.1 d (Cherepashchuk 1981). The uniqueness of this source comes from the presence of narrow oppositely directed subrelativistic jets emitting red and blue‐shifted periodically variable lines.…”

Highly evolved close binary systems

“…Highly evolved close binary systems 37 In the case of conservative mass exchange, for J orb = constant and m 1 + m 2 = constant, we obtain…”

“…The SS433 binary system is a high-mass X-ray binary at an advanced evolutionary stage, in which the optical star overfills its Roche lobe [37,38] and a supercritical accretion disc is formed around the relativistic object [39]. Therefore, intensive secondary mass exchange occurs in SS433 (Ṁ ≈ 10 −4 M year −1 ) and this unique HMCBS may be considered as a precursor of a WR + C binary.…”