Detailed photoionization and radiative acceleration of self-similar magnetocentrifugal accretion disk winds are explored .
First , a general-purpose hybrid magnetocentrifugal and radiatively-driven wind model is defined .
Solutions are then examined to determine how radiative acceleration modifies magnetocentrifugal winds and how those winds can influence radiative driving in Active Galactic Nuclei ( AGNs ) .
For the models studied here , both radiative acceleration by bound-free ( “ continuum-driving ” ) and bound-bound ( “ line-driving ” ) processes are found to be important , although magnetic driving dominates the mass outflow rate for the Eddington ratios studied ( L / L _ { Edd } = 0.001 - 0.1 ) .
The solutions show that shielding by a magnetocentrifugal wind can increase the efficiency of a radiatively-driven wind , and also that , within a magnetocentrifugal wind , radiative acceleration is sensitive to both the column in the shield , the column of the wind and the initial density at the base of the wind .