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An accretion disk in an Active Galactic Nucleus (AGN) harbors and shieldsdust from external illumination: at the mid-plane of the disk around a $M_{{\rmBH}}=10^{7}M_{\odot}$ black hole, dust can exist at $0.1$pc from the blackhole, compared to 0.5pc outside of the disk. We construct a physical model of adisk region approximately located between the radius of dust sublimation at thedisk mid-plane and the radius at which dust sublimes at the disk surface. Ourmain conclusion is that for a wide range of model parameters such as localaccretion rate and/or opacity, the accretion disk's own radiation pressure ondust significantly influences its vertical structure. In addition to beinghighly convective, such a disk can transform from geometrically thin to slim.Our model fits into the narrative of a "failed wind" scenario of Czerny &Hryniewicz (2011) and the "compact torus" model of Baskin & Laor (2018),incorporating them as variations of the radiative dusty disk model.

A physical model for radiative, convective dusty disk in AGN