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) for details of Compton reflection. See Fabian et al. (1989) for details of the disk line profile.
par1 | ![]() ![]() |
par2 | ![]() ![]() |
par3 | ![]() |
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,
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par10 | ![]() ![]() |
par11 | inner radius (units of ![]() |
par12 | outer radius (units of ![]() |
par13 | internal model accuracy - points of spectrum per energy decade |
norm | photon flux at 1 keV (photons/keV/cm![]() |