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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 proportional to E^-Gamma

par2

Ec, cutoff energy (keV) (if E_c = 0there is no cutoff)

par3

relrefl, reflection scaling factor (0, no direct component < relrefl < 1 for 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/n, where Fion 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 proportional to R^par10

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 keV1cm-2 s-1) of the cutoff broken power-law only (no reflection) in the observed frame.

 

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Next: Rnei Up: Additive Model Components Previous: Redge