Broken power-law spectrum multiplied by exponential high-energy cutoff, exp(-E/E_{c}), and reflected from ionized material. See Magdziarz & Zdziarski 1995, MNRAS, 273, 837 for details. Ionization and opacities of the reflecting medium is computed as in the absori model. The output spectrum is the sum of an e-folded broken power law and the reflection component. The reflection component alone can be obtained for _{}. Then the actual reflection normalization is _{}. Note that you need to change then the limits of _{} excluding zero (as then the direct component appears). If E_{c} = 0, there is no cutoff in the power law. The metal and iron abundances are variable with respect to those set by the command abund.
The core of this model is a Greens' function integration with one numerical integral performed for each model energy. The numerical integration is done using an adaptive method which continues until a given estimated fractional precision is reached. The precision can be changed by setting BEXRIV_PRECISION eg xset BEXRIV_PRECISION 0.05. The default precision is 0.01 (ie 1%).
par1 |
_{}, first power law photon index |
par2 |
E_{break}, break energy (keV) |
par3 |
_{}, second power law photon index |
par4 |
E_{c}, the e-folding energy in keV (if E_{c} = 0 there is no cutoff) |
par5 |
rel_{refl}, reflection scaling factor (1 for isotropic source above disk) |
par6 |
redshift, z |
par7 |
abundance of elements heavier than He relative to the solar abundances |
par8 |
iron abundance relative to the above |
par9 |
cosine of inclination angle |
par10 |
disk temperature, K |
par11 |
disk ionization parameter, _{}, where F_{ion} is the 5eV–20 keV irradiating flux, n is the density of the reflector; see Done et al., 1992, ApJ, 395, 275} |
norm |
photon flux at 1 keV of the cutoff broken power-law only (no reflection) in the observed frame.} |