  Recent simulations have demonstrated the formation of 'flux-frozen' and
hyper-magnetized disks, qualitatively distinct from both classical $\alpha$
disks and magnetically-arrested disks, as a natural consequence of fueling gas
to supermassive black holes in galactic nuclei. We previously showed that the
dynamical structure of said disks can be approximated by simple analytic
similarity models. Here we study the thermal properties of these models over a
wide range of physical scales and accretion rates. We show there are several
characteristic zones: a dusty 'torus'-like region, a multi-phase neutral and
then multi-phase ionized, broad line-emitting region interior to the
sublimation radius, before finally a transition to a thermal accretion disk
with a warm Comptonizing layer. The disks are strongly-flared with large scale
heights, and reprocess and/or scatter an order-one fraction of the central disk
emission. As a result, this simple accretion disk model predicts phenomena
including the existence of a dusty torus and its covering factor, geometry,
clumpiness, and dust temperatures; a broad-line-region (BLR) with its
characteristic sizes and luminosities and ionization properties; extended
scattering/reprocessing surfaces producing cooler disk continuum and apparently
large observed disk sizes; and existence of warm Comptonizing layers and hard
coronal gas. Remarkably, these properties emerge without our having to
introduce new components or parameters: they are all part of the accretion flow
if the disks are in the hyper-magnetized limit.
