
par1  eta, ratio of the disk power produced by a torque at the disk inner boundary to the disk power arising from accretion. It must be and . When eta = 0, the solution corresponds to that of a standard Keplerian disk with zero torque at the inner boundary. 
par2  specific angular momentum of the black hole in units of the black hole mass M (geometrized units G=c=1). Should be and <1. 
par3  disk's inclination angle (the angle between the axis of the disk and the line of sight). It is expressed in degrees. i=0 is for a "faceon" accretion disk. i should be degree. 
par4  the mass of the black hole in units of the solar mass. 
par5  the “effective” mass accretion rate of the disk in units of g/s. When eta = 0 (zero torque at the inner boundary), this is just the mass accretion rate of the disk. When eta is nonzero, the effective mass accretion rate = (1+eta) times the true mass accretion rate of the disk. The total disk luminosity is then “epsilon” times “the effective mass accretion rate” times c, where epsilon is the radiation efficiency of a standard accretion disk around the Kerr black hole 
par6  the distance from the observer to the black hole in units of kpc. 
par7  spectral hardening factor, T/T. It should be greater than 1.0, and considered to be 1.51.9 for accretion disks around a stellarmass black hole. See, e.g., Shimura & Takahara (1995) 
par8  a flag to switch on/off the effect of selfirradiation (never allowed to be free). Selfirradiation is included when > 0. Selfirradiation is not included when . 
par9  a flag to switch on/off the effect of limbdarkening (never allowed to be free). The disk emission is assumed to be limbdarkened when >0. The disk emission is assumed to be isotropic when lflag is . 
K  normalization. Should be set to 1 if the inclination, mass and distance are frozen. 
Parameters for zkerrbb:
par1  eta, ratio of the disk power produced by a torque at the disk inner boundary to the disk power arising from accretion. It must be and . When eta = 0, the solution corresponds to that of a standard Keplerian disk with zero torque at the inner boundary. 
par2  specific angular momentum of the black hole in units of the black hole mass M (geometrized units G=c=1). Should be and <1. 
par3  disk's inclination angle (the angle between the axis of the disk and the line of sight). It is expressed in degrees. i=0 is for a "faceon" accretion disk. i should be degree. 
par4  the mass of the black hole in units of the solar mass. 
par5  the “effective” mass accretion rate of the disk in units of /yr. When eta = 0 (zero torque at the inner boundary), this is just the mass accretion rate of the disk. When eta is nonzero, the effective mass accretion rate = (1+eta) times the true mass accretion rate of the disk. The total disk luminosity is then “epsilon” times “the effective mass accretion rate” times c, where epsilon is the radiation efficiency of a standard accretion disk around the Kerr black hole 
par6  the redshift of the black hole. 
par7  spectral hardening factor, T/T. It should be greater than 1.0, and considered to be 1.51.9 for accretion disks around a stellarmass black hole. See, e.g., Shimura & Takahara (1995) 
par8  a flag to switch on/off the effect of selfirradiation (never allowed to be free). Selfirradiation is included when > 0. Selfirradiation is not included when . 
par9  a flag to switch on/off the effect of limbdarkening (never allowed to be free). The disk emission is assumed to be limbdarkened when >0. The disk emission is assumed to be isotropic when lflag is . 
K  normalization. Should be set to 1 if the inclination, mass and distance are frozen. 
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