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kerrbb: multi-temperature blackbody model for thin accretion disk around a Kerr black hole

A multi-temperature blackbody model for a thin, steady state, general relativistic accretion disk around a Kerr black hole. The effect of self-irradiation of the disk is considered, and the torque at the inner boundary of the disk is allowed to be non-zero. This model is intended as an extension to grad, which assumes that the black hole is non-rotating. For details see Li et al., ApJSuppl, 157, 335, 2005.

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 $\geq 0$ and $\leq 1$. 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 $\geq -1$ 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 "face-on" accretion disk. i should be $\leq 85$ 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 $10^{18}$ 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$^2$, 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$_{col}$/T$_{eff}$. It 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 and Takahara 1995, ApJ, 445, 780
par8 a flag to switch on/off the effect of self-irradiation (never allowed to be free). Self-irradiation is included when > 0. Self-irradiation is not included when $\leq 0$.
par9 a flag to switch on/off the effect of limb-darkening (never allowed to be free). The disk emission is assumed to be limb-darkened when >0. The disk emission is assumed to be isotropic when lflag is $\leq 0$.
K normalization. Should be set to 1 if the inclination, mass and distance are frozen.


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Next: kerrd: optically thick accretion Up: Additive Model Components Previous: hatm: Nonmagnetic hydrogen atmosphere