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kyconv: convolution using a relativistic line from axisymmetric accretion disk

Convolution using as a kernel the relativistic line from an axisymmetic accretion disk. See Dovciak et al. (2004).

par1 a/M; BH angular momentum (GM/c)
par2 theta_o; observer inclination (0 = pole on, degrees)
par3 rin; inner radius (GM/c$^2$)
par4 ms; 0 means integrate from rin, 1 means integrate emission from above the marginally stable orbit only
par5 rout; outer radius (GM/c$^2$)
par6 alpha; accretion disk emissivity scales as $r^{-alpha}$ for $r<rb$
par7 beta; accretion disk emissivity scales as $r^{-beta}$ for $r>rb$
par8 rb; boundary radius between inner and outer emissivity laws (GM/c$^2$)
par9 zshift; overall Doppler shift
par10 limb; 0 means isotropic emission, 1 means Laor's limb darkening ($1+0.26\mu$), 2 means Haardt's limb brightening ($\ln{1+1/\mu}$
par11 ne_loc; number of grid points in local energy (energy resolution of local flux, the grid is equidistant in logarithmic scale)
par12 normal; 0 means normalize total flux to unity, +ve value means normalize to unity at the energy given by the parametervalue, -ve value means unnormalized.


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Next: lsmooth: lorentzian smoothing Up: Convolution Model Components Previous: kerrconv: accretion disk line