  The Broad Line Region (BLR) in AGN is composed of dense gas ($\sim 10^{11}$
cm$^{-3}$) on sub-pc scale, which absorbs about 30 per cent of the ionising
continuum. The outer size of the BLR is likely set by dust sublimation, and its
density by the incident radiation pressure compression (RPC). But, what is the
origin of this gas, and what sets its covering factor (CF)? Czerny & Hryniewicz
(2011) suggested that the BLR is a failed dusty wind from the outer accretion
disc. We explore the expected dust properties, and the implied BLR structure.
We find that graphite grains sublimate only at $T\simeq 2000$ K at the
predicted density of $\sim 10^{11}$ cm$^{-3}$, and therefore large graphite
grains ($\ge 0.3$ $\mu$m) survive down to the observed size of the BLR, $R_{\rm
BLR}$. The dust opacity in the accretion disc atmosphere is $\sim 50$ times
larger than previously assumed, and leads to an inflated torus-like structure,
with a predicted peak height at $R_{\rm BLR}$. The illuminated surface of this
torus-like structure is a natural place for the BLR. The BLR CF is mostly set
by the gas metallicity, the radiative accretion efficiency, a dynamic
configuration, and ablation by the incident optical-UV continuum. This model
predicts that the BLR should extend inwards of $R_{\rm BLR}$ to the disc radius
where the surface temperature is $\simeq 2000$ K, which occurs at $R_{\rm
in}\simeq 0.18 R_{\rm BLR}$. The value of $R_{\rm in}$ can be tested by
reverberation mapping of the higher ionisation lines, predicted by RPC to peak
well inside $R_{\rm BLR}$. The dust inflated disc scenario can also be tested
based on the predicted response of $R_{\rm BLR}$ and the CF to changes in the
AGN luminosity and accretion rate.
