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SLIMBH is a relativistic model for X-ray continuum of stationary slim accretion disks around stallar mass black holes. This model is based on disk radial structure solutions presented in Sadowski et al. 2010 combined with vertical structure computed using TLUSTY code to make the best model for X-ray continuum for a wide range of luminosities up to Eddington limit. See also Straub et al. 2011.

Model parameters

par# name description
par1 M mass of the black hole (in solar units)
par2 a black hole spin parameter (dimensionless; 0
par3 L luminosity (total disk luminosity in Eddington units)
par4 alpha alpha-viscosity
par5 i inclination (in degrees; 0
par6 D distance to the source (in kpc)
par7 f hardening factor; negative value means to use TLUSTY spectra
par8 l_flag lflag, a flag to switch on/off the effect of limb-darkening (not allowed to be free). If positive, disk emission is limb-darkened; if
par9 z_flag switch on/off surface profile; if positive, raytracing is done from the actual photosphere; if
par10 K normalization; should be fixed to 1


The model requires a FITS table with pre-computed spectral data.
FITS table download link: slimbb-full.fits


The following plot shows a comparison between SLIMBH spectrum (red) and relativistic thin disk spectrum (blue) for a 10 M_Sun black hole with spin a=0.9 and disk luminosity L=0.5 L_Edd.

SLIMBH vs. KERRBB spectrum