kerrd: optically thick accretion disk around a Kerr black hole

Optically thick extreme-Kerr disk model based on the same tranfer-function used in the laor Kerr disk-line model. Local emission is simply assumed to be the diluted blackbody. See Laor (1991) for an explanation of the transfer function. See Ebisawa et al. (2003) for examples of using this model.

par1	distance (kpc)
par2	spectral hardening factor, Tcol/Teff. Should be greater than 1.0, and considered to be 1.5–1.9 for accretion disks around a stellar-mass black hole. See, e.g., Shimura & Takahara (1995) 445, 780
par3	mass of the central object (solar unit)
par4	mass accretion rate ($10^{18}$ g/s)
par5	disk inclination angle (deg; 0 for face-on)
par6	inner radius (units of $GM/c^2$). 1.235 is the last stable orbit.
par7	outer radius (units of $GM/c^2$)
K	normalization factor. should be fixed to 1.

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Last modified: Friday, 23-Aug-2024 13:20:40 EDT