INTEGRAL observations of SS433: system's parameters and nutation of supercritical accretion disc

Черепащук, А. М.; Sunyaev, R.; Molkov, S.; Antokhina, É. A.; Постнов, К. А.; Bogomazov, A. I.

doi:10.1093/mnras/stt1715

Cited by 32 publications

(45 citation statements)

References 39 publications

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“…(Rico 2008;Cherepashchuk et al 2013;Staubert et al 2013 and references therein), and are typically assumed to be related to precession of the accretion flow analogous to that seen in SS433, for which this interpretation is well established (Fabrika 2004). However, super-orbital periods have also now been seen in wind-fed high-mass X-ray binaries, for which such a scenario is unlikely to be viable (Corbet & Krimm 2013), and other, more exotic mechanisms such as triple systems have been proposed in some cases (see Kotze & Charles 2012 for a recent review of super-orbital variability in X-ray binaries).…”

Section: Discussionmentioning

confidence: 99%

A 78 Day X-Ray Period Detected From NGC 5907 Ulx1 by Swift

Walton

Fürst

Bachetti

et al. 2016

ApJL

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We report the detection of a 78.1 ± 0.5 day period in the X-ray light curve of the extreme ultraluminous X-ray source NGC 5907 ULX1 ( L X,peak ∼ 5 × 10 40 erg s−1), discovered during an extensive monitoring program with Swift. These periodic variations are strong, with the observed flux changing by a factor of ∼3–4 between the peaks and the troughs of the cycle; our simulations suggest that the observed periodicity is detected comfortably in excess of 3σ significance. We discuss possible origins for this X-ray period, but conclude that at the current time we cannot robustly distinguish between orbital and super-orbital variations.

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Section: Discussionmentioning

confidence: 99%

A 78 Day X-Ray Period Detected From NGC 5907 Ulx1 by Swift

Walton

Fürst

Bachetti

et al. 2016

ApJL

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“…The analysis of hard X-ray eclipses in SS433 (20-60 keV) observed by INTEGRAL with an account for the precession flux variability suggests the component mass ratio q 0.3 (Cherepashchuk et al 2013). In this analysis, the optical star was assumed to fill its Roche lobe and to eclipse an extended quasi-isothermal hot corona above the accretion disc.…”

Section: The Mass Ratio Estimate From the Analysis Of X-ray Eclipsesmentioning

confidence: 99%

On masses of the components in SS433

Cherepashchuk

Постнов

Belinski

2018

Monthly Notices of the Royal Astronomical Society

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A huge optical luminosity of the supercritical accretion disc and powerful stellar wind in the high-mass X-ray binary SS433 make it difficult to reliably estimate the mass ratio of the binary components from spectroscopic observations. We analyze different indirect methods of the mass ratio estimate. We show that with an account of the possible Roche lobe overflow by the optical star, the analysis of X-ray eclipses in the standard and hard X-ray bands suggests the estimate q = M x /M v 0.3. We argue that the double-peak hydrogen Brackett lines in SS433 should form not in the accretion disc but in a circumbinary envelope, suggesting a total mass of M v + M x 40M . The observed long-term stability of the orbital period in SS433 | P b /P b | ≤ 1.793 × 10 −14 s −1 over ∼ 28 year period is used to place an independent constraint of q 0.6 in SS433, confirming its being a Galactic microquasar hosting a superaccreting black hole.

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“…b The seed photon temperature kT 0 is locked to the peak temperature of the disk, kT in . on a 13.1 day binary period (e.g., Stewart et al 1987;Fabrika 2004;Brinkmann et al 2005;Kubota et al 2010;Cherepashchuk et al 2013;Marshall et al 2013). Unlike M51 ULX-1 and ULX-2, SS 433 does not appear as luminous as a ULX because the direct X-ray emission from the inner-disk/ corona region is already occulted from us.…”

Section: Table 11mentioning

confidence: 99%

Two Eclipsing Ultraluminous X-Ray Sources in M51

Urquhart

Soria

2016

ApJ

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We present the discovery, from archival Chandra and XMM-Newton data, of X-ray eclipses in two ultraluminous X-ray sources (ULXs), located in the same region of the galaxy M51: CXOM51 J132940.0+471237 (ULX-1, for simplicity) and CXOM51 J132939.5+471244 (ULX-2). Three eclipses were detected for ULX-1 and two for ULX-2. The presence of eclipses puts strong constraints on the viewing angle, suggesting that both ULXs are seen almost edge-on and are certainly not beamed toward us. Despite the similar viewing angles and luminosities ( »Ĺ 2 10 X 39 erg s −1 in the 0.3-8 keV band for both sources), their X-ray properties are different. ULX-1 has a soft spectrum, well fitted by Comptonization emission from a medium with electron temperature » kT 1 keV e . ULX-2 is harder, well fitted by a slim disk with » kT 1.5 in -1.8 keV and normalization consistent with a ∼10 M e black hole. ULX-1 has a significant contribution from multi-temperature thermal-plasma emission ( »Ĺ 2 10 X,mekal 38 erg s −1 ). About 10% of this emission remains visible during the eclipses, proving that the emitting gas comes from a region slightly more extended than the size of the donor star. From the sequence and duration of the Chandra observations in and out of eclipse, we constrain the binary period of ULX-1 to be either »6.3 days, or ≈12.5-13 days. If the donor star fills its Roche lobe (a plausible assumption for ULXs), both cases require an evolved donor, most likely a blue supergiant, given the young age of the stellar population in that Galactic environment.

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INTEGRAL observations of SS433: system's parameters and nutation of supercritical accretion disc

Cited by 32 publications

References 39 publications

A 78 Day X-Ray Period Detected From NGC 5907 Ulx1 by Swift

A 78 Day X-Ray Period Detected From NGC 5907 Ulx1 by Swift

On masses of the components in SS433

Two Eclipsing Ultraluminous X-Ray Sources in M51

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