Accretion Disk Spectra of Ultra-luminous X-ray Sources and Galactic Superluminal Jet Sources

Details Accretion Disk Spectra of Ultra-luminous X-ray Sources and Galactic Superluminal Jet Sources Accretion Disk Spectra of Ultra-luminous X-ray Sources and Galactic Superluminal Jet Sources

Nov 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002xrb..confe...7e&link_type=abstract

X-ray Binaries in the Chandra and XMM-Newton Era (with an emphasis on Targets of Opportunity), Abstracts of the conference held

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Actively Accreting And Transient Binaries

Scientific paper

The Ultra-luminous X-ray Sources (ULXs) in nearby spiral galaxies and Galactic superluminal jet sources share a similar spectral property that they have unusually high disk temperatures which cannot be explained in the framework of the standard accretion disk model in the Schwarzschild metric. We have calculated an extreme Kerr disk model to fit the observed spectra of ULXs and superluminal jet sources, in order to examine the claim that the Kerr disk may explain the observed high disk temperature, as the inner radius can be smaller and the disk will be hotter than in the Schwarzschild case. We have found that the observed Kerr disk spectra become significantly harder compared to the Schwarzschild disk due to the Doppler boosts in the very vicinity of the black hole, only when the disk is highly inclined. Consequently, the Kerr disk model may be appropriate for superluminal jet sources, which are known to be highly inclined systems. For ULXs, on the other hand, the Kerr disk interpretation is problematic, as it is highly unlikely that their accretion disks are preferentially inclined. Instead, the slim disk (advection dominated optically thick disk) model is likely to explain the observed super- Eddington luminosities and hard spectra of ULXs.

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