|README.md||Loading commit data...|
|initslimbb.xcm||Loading commit data...|
|lmodel_slimbb.dat||Loading commit data...|
|xslimbb.c||Loading commit data...|
|xslimbb.h||Loading commit data...|
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.
|par1||M||mass of the black hole (in solar units)|
|par2||a||black hole spin parameter (dimensionless; 0<a<0.999)|
|par3||L||luminosity (total disk luminosity in Eddington units)|
|par5||i||inclination (in degrees; 0<=i<=85)|
|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 <=0, disk emission is assumed to be isotropic|
|par9||z_flag||switch on/off surface profile; if positive, raytracing is done from the actual photosphere; if <=0, spectrum is raytraced from the equatorial plane ignoring the height profile of the disk|
|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.