X-ray radiation of the jets and the supercritical accretion disk in SS 433

Abstract

Abstract. The observed X-ray luminosity of SS 433 is ∼ 10 36 erg/s, it is known that all the radiation is formed in the famous SS 433 jets. The bolometric luminosity of SS 433 is ∼ 10 40 erg/s, and originally the luminosity must be realized in X-rays. The original radiation is probably thermalized in the supercritical accretion disk wind, however the missing more than four orders of magnitude is surprising. We have analysed the XMM-Newton spectra of SS 433 using a model of adiabatically and radiatively cooling X-ray jets. The multi-temperature thermal jet model reproduces very well the strongest observed emission lines, but it can not reproduce the continuum radiation and some spectral features. We have found a notable contribution of ionized reflection to the spectrum in the energy range from ∼ 3 to 12 keV. The reflected spectrum is an evidence of the supercritical disk funnel, where the illuminating radiation comes from deeper funnel regions, to be further reflected in the outer visible funnel walls (r 2 · 10 11 cm). The illuminating spectrum is similar to that observed in ULXs, its luminosity has to be no less than ∼ 10 39 erg/s. A soft excess has been detected, that does not depend on the thermal jet model details. It may be represented as a BB with a temperature of T bb ≈ 0.1 keV and luminosity of L bb ∼ 3 · 10 37 erg/s. The soft spectral component has about the same parameters as those found in ULXs.

Supercritical Accretion Discs in Ultraluminous X-ray Sources and SS 433

“…We finally examine if the optical spectra of our ULXs can be explained by a supercritical accretion disc (SCAD) with a stellar-mass black hole. Indeed, the only known supercritical accretor SS 433 shows a similar optical spectrum to ours, which is produced by the disc wind from the SCAD 3 . In SS 433 the He II line is narrower than Hα 10,24 .…”

“…The spectra are also similar to that of SS 433 10 , the only known supercritical accretor in our Galaxy, a close binary consisting of an A-type supergiant and a stellar-mass black hole. SS 433 apparently exhibits a WNL-type spectrum 3,11 because the physical conditions of its disc wind may be similar to those of stellar winds from WNL stars. The impression of the spectral similarity is strengthened because the absolute visual magnitudes of both WNLs and SS 433 are in the same range as in the ULX counterparts 6,12 (Fig.…”

Modelling the light curves of ultraluminous X-ray sources as precession

“…As mentioned in the previous section, velocities of the outflow are expected to be in the range of v ≈ 0.2-0.4 c and we consider a height of the cone of 1000 rg as plausible. Note that even much larger values have been suggested for SS433 (Fabrika & Medvedev 2011). Currently there do not exist any constraints on the opening angle of such a cone.…”

A newly discovered double–double candidate microquasar in NGC 300

“…Three possibly super-Eddington microquasars have been found so far with large-scale X-ray evidence of collimated jets: NGC 300 S 10, NGC 7793 S 26 and SS 433 in the Milky Way. Curiously, all three have apparently faint cores: L X,core 10 36 erg s −1 (Section 3.1.2), L X,core ≈ 6 × 10 36 erg s −1 ) and ∼ 10 36 erg s −1 (Kotani et al 1996;Fabrika & Medvedev 2011) for the three sources, respectively. In the case of SS 433, the reason is the occultation of the direct X-ray emission by the thick super-critical disk, seen at high inclination (Fabrika 2004).…”