The High‐Resolution X‐Ray Spectrum of SS 433 Using the<i>Chandra</i>HETGS

Marshall, Herman L.; Canizares, C. R.; Schulz, Norbert S.

doi:10.1086/324398

Cited by 166 publications

(247 citation statements)

References 15 publications

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“…This would explain that there is no evidence for an accretion disc in the Chandra X-ray spectrum of SS 433 according to Marshall et al (2002) and that SS 433 is not as strong an X-ray source as the other microquasars or Xray transients.…”

Section: A Phenomenon Imitating a Wolf-rayet Starmentioning

confidence: 98%

SS 433: a phenomenon imitating a Wolf-Rayet star

Fuchs

Miramond

Ábrahám

2006

A&A

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We present mid-infrared (2-12 µm) spectra of the microquasar SS 433 obtained with the Infrared Space Observatory (spectroscopic mode of ISOPHOT and ISOCAM). We compare them to the spectra of four Wolf-Rayet stars: WR 78, WR 134, WR 136, and WR 147 in the same wavelength range. The mid-infrared spectrum of SS 433 mainly shows H i and He i emission lines and is very similar to the spectrum of WR 147, a WN8(h)+B0.5V binary. The 2-12 µm continuum emission of SS 433 corresponds to optically thin and partially optically thick free-free emission, from which we calculate a mass loss rate of 2−3 × 10 −4 M yr −1 if the wind is homogeneous and a third of these values if it is clumped. This is consistent with a strong stellar wind from a WN star. However, following recent studies concluding that the mass donor star of SS 433 is not a Wolf-Rayet star, we propose that this strong wind out flows from a geometrically thick envelope of material that surrounds the compact object like a stellar atmosphere, imitating the Wolf-Rayet phenomenon. This wind could also wrap the mass donor star, and at larger distances (∼40 AU), it might form a dust envelope from which the thermal emission, detected with ISOPHOT at 25 µm and 60 µm, would originate. This wind also probably feeds the material that is ejected in the orbital plane of the binary system and that forms the equatorial outflow detected in radio at distances > 100 AU.

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Section: A Phenomenon Imitating a Wolf-rayet Starmentioning

confidence: 98%

SS 433: a phenomenon imitating a Wolf-Rayet star

Fuchs

Miramond

Ábrahám

2006

A&A

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“…The observed X-ray luminosity of SS 433 is ∼ 10 36 erg/s and it is believed that all the X-rays come from the cooling X-ray jets (Kotani et al 1996;Marshall, Canizares, & Schulz 2002;Brinkmann, Kotani, & Kawai 2005). The observed X-ray radiation is at least four orders of magnitude less than the bolometric luminosity, which originally must be released in X-rays.…”

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confidence: 99%

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

Fabrika¹,

Medvedev²

2010

Proc. IAU

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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.

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“…The jet interpretation of the radio emission was confirmed by the milliarcseconds scale jets observed in Cygnus X-1 (Stirling et al 2001) and GRS 1915+105 (Dhawan et al 2000). In X-ray band, arcsecond scale jets have been observed for the first time in SS 433 with the Chandra X-ray observatory (Marshall et al 2002). For microquasars 1E1740.7-2942, a broad emission line detected by SIGMA has been reported (Sunyaev et al 1991).…”

Section: Discussionmentioning

confidence: 75%

Searching for the 511 keV annihilation line from galactic compact objects with the IBIS gamma ray telescope

Cesare¹

2011

A&A

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Context. The first detection of a gamma ray line with an energy of about 500 keV from the center of our Galaxy dates back to the early seventies. Thanks to the astrophysical application of high spectral resolution detectors, it was soon clear that this radiation was due to the 511 keV photons generated by electron-positron annihilation. Even though the physical process are known, the astrophysical origin of this radiation is still a mystery. Aims. The spectrometer SPI aboard the INTEGRAL gamma-ray satellite has been used to produce the first all-sky map in light of the 511 keV annihilation, but no direct evidence of any 511 keV galactic compact objects has been found. Owing to its moderate angular resolution, these SPI data are still compatible with a distribution of point sources clustered in the bulge of our Galaxy. Thanks to the fine angular resolution and the large field of view, the IBIS imager on the INTEGRAL satellite gives us the unique opportunity to search for a possible 511 keV line from point sources associated to known objects, such as X-ray binaries, or supernovae, or even new ones. Methods. We present the first deep IBIS 511 keV all-sky map, obtained by applying standard analysis to about 5 years of data. Possible 511 keV signals are also searched over hour-day-month timescales. The IBIS sensitivity at 511 keV depends on the detector quantum efficiency at this energy and on the background. Both these quantities were estimated in this work. Results. We find no evidence of Galactic 511 keV point sources. With an exposure of 10 Ms, in the center of the Galaxy, we estimate a 1.6 × 10 −4 ph cm −2 s −1 flux 2 sigma upper limit. A similar limit is given in a wide area in the Galactic center region with similar exposures. The IBIS 511 keV flux upper limits for microquasars and supernova remnants detected in the hard X domain (E > 20 keV) are also reported. Conclusions. Our results are consistent with a diffuse e + e − annihilation scenario. If positrons are generated in compact objects, we expect that a significant fraction of them propagate in the interstellar medium before they are annihilated away from their birth places.

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The High‐Resolution X‐Ray Spectrum of SS 433 Using theChandraHETGS

Cited by 166 publications

References 15 publications

SS 433: a phenomenon imitating a Wolf-Rayet star

SS 433: a phenomenon imitating a Wolf-Rayet star

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

Searching for the 511 keV annihilation line from galactic compact objects with the IBIS gamma ray telescope

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