Spectra From Relativistic Accretion Disk

In this paper, under full general relativity, we study structure of slim accretion disks, as well as their observational behavior. Slim disk is a branch of accretion disk which exists in highly accreting systems. In this work, we focus on the dynamical property of slim accretion disks, as well as the observational consequence, which in-clude the disk blackbody emission as well as the 6.4 KeV broad Fe Kαline emission. We found that the disk dynamics and the self-shadowing effect influence the observed spectra for relatively high accretion rate(L> 0.2LEdd)-For the disk blackbody emis-sion, we found that both the disk dynamics and the self-shadowing of the accretion disk have significant effect on the emergent spectra, especially at the high energy part. Since the spin determination relies on the fitting of the disk spectra, according to our result, this spin determination may still be inaccurate as a result. For the broad iron line emission, we found that for system with high accretion rate, there is no abrupt change of physical properties of the accretion disk around the ISCO. As a result, fitting the broad relativistic iron line may not be able to constrain the spin of the black hole in this case. By analyzing current data, we found strong evidence that the self-shadowing effect is at work. Implications for interpretation of observed spectra for single sources and statistical analysis of large data samples are discussed.