![black hole accretion disk xray black hole accretion disk xray](https://3c1703fe8d.site.internapcdn.net/newman/gfx/news/hires/2013/jhgyg.jpg)
) 157–213 (Cambridge Astrophysics Series No. in Compact Stellar X-ray Sources (eds Lewin, W. Multi-epoch multi-wavelength study of an ultraluminous X-ray source in M101: the nature of the secondary. Mukai, K., Still, M., Corbet, R., Kuntz, K. An ultraluminous supersoft X-ray source in M81: an intermediate-mass black hole? Astrophys. Evidence of an intermediate-mass black hole: Chandra and XMM-Newton observations of the ultraluminous supersoft X-ray source in M101 during its 2004 outburst. A comparison of intermediate mass black hole candidate ultraluminous X-ray sources and stellar mass black holes. The sub-classes of ultraluminous X-ray sources. The hunt for intermediate-mass black holes. Accretion must occur from captured stellar wind, which has hitherto been thought to be so inefficient that it could not power an ultraluminous source 12, 13.įabbiano, G. Therefore, its exceptionally soft spectra at high Eddington ratios violate the expectations for accretion onto stellar-mass black holes 9, 10, 11. The black hole has a minimum mass of 5, and more probably a mass of 20 −30, but we argue that it is very unlikely to be an intermediate-mass black hole. We confirm the previous suggestion 8 that the system contains a Wolf-Rayet star, and reveal that the orbital period is 8.2 days. Here we report optical spectroscopic monitoring of M 101 ULX-1. On its discovery, M 101 ULX-1 4, 7 had a luminosity of 3 × 10 39 erg s −1 and a supersoft thermal disk spectrum with an exceptionally low temperature-uncomplicated by photons energized by a corona of hot electrons-more consistent with the expected appearance of an accreting intermediate-mass black hole 3, 4.
![black hole accretion disk xray black hole accretion disk xray](https://mcdonaldobservatory.org/sites/default/files/images/news/gallery/M87_BH.jpg)
Alternatively, they could be stellar-mass black holes radiating at Eddington or super-Eddington rates 2, 6. They could be intermediate-mass black holes (more than 100–1,000 solar masses, ) radiating at sub-maximal (sub-Eddington) rates, as in Galactic black-hole X-ray binaries but with larger, cooler accretion disks 3, 4, 5. There are two proposed explanations for ultraluminous X-ray sources 1, 2 (ULXs) with luminosities in excess of 10 39 erg s −1.