A convolution model to smooth a spectrum by relativistic effects from an accretion disk around a non-rotating black hole. Modified from diskline model (Fabian et al. (1989)) by Andy Fabian and Roderick Johnstone.
|par1||Index: power law dependence of emissivity (scales as ). If this parameter is 10 or greater then the accretion disk emissivity law is used.|
|par2||inner radius (units of )|
|par3||outer radius (units of )|