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# SLIMBH – XSPEC model

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

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)
par4 	alpha 	alpha-viscosity
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)

### Data
FITS table with spectral data: (slimbb-full.fits)[http://astro.cas.cz/bursa/projects/slimbb/slimbb-full.fits]

### Usage in XSPEC

### Example

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][http://astro.cas.cz/bursa/projects/slimbb/plot/slimbb-graph.php?mass=10&spin=0.99&lumi=0.5&alpha=0.1&incl=66&dist=10&hardf=1.7&plot%5BL0%5D=on&plot%5BSV%5D=on]