450 Hz QPO (Strohmayer 2001) also supports.Inclined Kerr disk model works to solve the too.Kerr disk model with a0.68 to 0.88 is consistent.Too small compared to M7 M? from optical.Schwarzschild disk model ? M1.8 M? (Ebisawa et.
Unusually high disk temperature (e.g., Zhang, Cui Highly inclined systems, and known to have Due to doppler boosts in the innermost regionĪpplication of Kerr disk spectra to GRO J1655-40.Edge-on Kerr disk has very hard spectrum.When the disk is face-on, relativistic effects do.Relativistic effects and inclination dependence.Inclined Kerr disk is brighter in high energies!Ĭomparison of Schwarzschild and Kerr disk spectra Hard spectra of microquasars may be explained.Inclined Kerr disk spectrum is significantly.Face-on Kerr disk spectrum is not very difference.Schwarzschild disk spectrum is not very different.Doppler effect, gravitational redshift, light.Kerr disk can be hotter than Schwarzschild disk.Innermost disk radius Last stable orbit.
Optically thick accretion disk Ldisk ? Rin2 Tin4ĭistance, inclination fixed, M, dM/dt free
Theoretical optically thick accretion disk.Optically thick accretion disk in the Soft state multi-color disk-blackbody approximation works.Standard accretion disk spectrum looks like.Luminosity (Shimura and Takahra 1995 Ross and Tcol/Teff 1.7-1.9 independent of radius and disk.Local emission shows Wien peak with Tcol(r).Comptonization is significant in the inner region.Gravitational energy is released as thermal.Standard disk is observationally established Slimĭisk seems to be observed in Galactic BHC and ULXs Of optically thick accretion disk spectra In this talk, I will concentrate on observation.2-10 keV X-ray spectrum is thermal (ultra-soft),.Galactic Black Hole Candidates Spectral States X-ray Observation of Black Hole Accretion Disks Title: Xray Observation of Black Hole Accretion Disks