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refsch: reflected power law from ionized accretion disk

Exponentially cut-off power-law spectrum reflected from an ionized relativistic accretion disk. In this model, spectrum of pexriv is convolved with a relativistic disk line profile diskline. See Magdziarz & Zdziarski 1995 MNRAS, 273, 837 for details of Compton reflection. See Fabian et al. 1989, MNRAS, 238, 729 for details of the disk line profile.

par1 $\Gamma$, power law photon index, $N_E \propto E^{-\Gamma}$
par2 $E_c$, cutoff energy (keV) (if $E_c = 0$ there is no cutoff)
par3 $rel_{refl}$, reflection scaling factor (0 = no direct component, 1 corresponds to an isotropic source above disk)
par4 redshift, z
par5 abundance of elements heavier than He relative to the solar abundances
par6 iron abundance relative to that defined by abund
par7 inclination angle (degrees)
par8 disk temperature in K
par9 disk ionization parameter, $\xi = 4\pi{F_{ion}\over{n}}$, where $F_{ion}$ is the 5eV - 20keV irradiating flux, $n$ is the density of the reflector; see Done et al., 1992, ApJ, 395, 275.
par10 $e$, power law dependence of emissivity. the emissivity $\propto R^e$
par11 inner radius (units of $GM/c^2$)
par12 outer radius (units of $GM/c^2$)
par13 internal model accuracy - points of spectrum per energy decade
norm photon flux at 1 keV (photons/keV/cm$^2$/s) of the cutoff broken power-law only (no reflection) in the observed frame.


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Next: rnei, vrnei, vvrnei: non-equilibrium Up: Additive Model Components Previous: redge: emission, recombination edge