We present a semianalytic model of steady-state magnetically and radiatively driven disk outflows in Active Galactic Nuclei consisting of a continuous wind with embedded clouds. The continuous outflow is launched from narrow sector on the disk surface as a centrifugally driven wind. Clouds are either uplifted from the disk by the ram pressure of the continuous outflow or are transient, created and destroyed throughout the wind. The inner regions of the outflow shield the outer portions from the strong ionizing central continuum, enabling gas in the outer regions to be radiatively accelerated. This thesis first describes the model in detail, outlines the tests used to verify its accuracy, and then compares it to other outflow models already in use. We present representative solutions of the model to explore the dependence of outflow properties on the relevant physical parameters, and also explore the impact of “ephemeral” (transient) condensations present throughout the wind vs. the disk-launched clouds introduced with the original model.; We find agreement with previous models where such comparisons are possible, although we also find that our more detailed radiative acceleration calculations do differ from some previous 2D hydrodynamical simulations. As in previous work, we find that radiative acceleration can have a significant impact on wind kinematics near the surface of the disk. We determine that continuum driving dominates line driving in the wind, whereas line driving accounts for most of the cloud acceleration. Also, when the winds contain dust, radiative acceleration can modify their terminal velocities by 80% over pure centrifugally-driven outflows. Finally, we find that only “ephemeral” clouds can substantially change the structure of the wind for M˙cloudM˙wind: condensations launched from the accretion disk rapidly accelerate out, of the thin wind and do not significantly affect the geometry or kinematics of the wind.
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