An emission line from an accreti on disk with a broken power-law emissivity profile around a black hole. Uses Ari Laor's calculation including GR effects (Laor (1991)). Modified from laor model by Andy Fabian.
|par1||Line energy in keV|
|par2||: power law dependence of emissivity (scales as )|
|par3||inner radius (units of )|
|par4||outer radius (units of )|
|par6||radius at which emissivity power-law index changes|
|par7||Emissivity power-law index for radii >par6|
|norm||photons/cm/s in the line|