The nature of SS433 and the ultraluminous X-ray sources
By M. Begelman, A. King, J. E. Pringle. 2006
188 citations recorded by the source corpus.
The periodic precession (162-d) and nodding (6.3-d) motions of the jets in SS433 are driven in the outer regions of the disc, whereas the jets themselves, being relativistic, are launched near the black hole at the disc centre. Given that the nutation period is comparable to the dynamical time-scale in the outer regions of the disc, it seems unlikely that these periods can be communicated efficiently to the disc centre. Here, we propose that the massive outflow observed in SS433 is launched at large radii in the disc, about 1/10 of the outer disc edge, and that it is this outflow which responds to the oscillations of the outer disc and determines the direction of the jets. The massive outflow is launched at large radius because the mass transfer rate is hyper-Eddington. This implies not only that the total luminosity of SS433 exceeds L Edd by a considerable factor, but also that the radiative output is collimated along the outflow. We thus suggest that SS433 is an ultraluminous X-ray source (ULX) viewed 'from the side'. We also suggest that the obscured INTEGRAL sources may be SS433-like objects, but with slightly lower mass transfer rates.
Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics
View Paper: https://www.semanticscholar.org/paper/a3fbef9264650ddc0e3e6efc5a7e61a6264c614c
How researchers see this paper
The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.
In Astronomy and Astrophysics
In Nuclear and High Energy Physics
Citations in the corpus
- Supercritically accreting stellar mass black holes as ultraluminous X-ray sources (2006, background): “…al. 1997) and a super-critical transient V4641 Sgr (Revnivtsev et al. 2002), show optical spectra with characteristic temperatures of 30 000–50 000 K, which we associate with the emission from the outer photosphere (and not with the spherization temperatureTsp as proposed by Begelman et al. 2006).”
- A GLOBAL THREE-DIMENSIONAL RADIATION MAGNETO-HYDRODYNAMIC SIMULATION OF SUPER-EDDINGTON ACCRETION DISKS (2014, background): “This so called butterfly diagram has been observed widely in local shearing box (Stone et al. 1996; Miller & Stone 2000; Shi et al. 2010; Davis et al. 2010; Jiang et al. 2014b) and global simulations (O’Neill et al. 2011).”
- On the diffusive propagation of warps in thin accretion discs (2010, background): “Observationally, warps are found in galactic binary system, such as the hyperaccreting X-ray binary SS433 (Begelman et al. 2006) and the X-ray binary Her X-1 (Wijers & Pringle 1999), and in several microquasars, including GRO J1655-40 (Martin etal.”
- The Ultraluminous State (2009, methodology): “There are two ways to do this, either by changing the mass accretion rate as a function of radius through expelling the excess mass via winds (Shakura & Sunyaev 1973; Begelman et al. 2006) or by changing the radiativeefficiency by advecting the photons along with the flow (slim discs, as above).”
- Ultraluminous X-ray sources in the Chandra and XMM-Newton era (2011, background): “In the simplest outflow scenario, Rin ∼ ṁ (Begelman et al. 2006; Poutanen et al. 2007).”
- Forming short-period Wolf–Rayet X-ray binaries and double black holes through stable mass transfer (2017, background): “The total mass loss from the disk is basically all the matter that the A-supergiant donor is transferring to the compact object by Roche-lobe overflow on its thermal timescale of ∼ 105 years (see also Begelman et al. 2006).”
- Modelling the behaviour of accretion flows in X-ray binaries (2007, background): “However, the clear signatures of mass loss seen from this system (Kotani et al. 2000; Lee et al. 2002) also point to additional cooling from winds being important, as expected for L ≥ LEdd (e.g. Shakura & Sunyaev 1973; Begelman et al 2006; Ohsuga 2006; 2007; Poutanen et al. 2007).”