  Protoplanetary disks are strongly irradiated by a stellar FUV spectrum that
is dominated by Ly$\alpha$ photons. We investigate the impact of stellar
Ly$\alpha$ irradiation on the terrestrial planet region of disks ($\lesssim
1$AU) using an updated thermal-chemical model of a disk atmosphere irradiated
by stellar FUV and X-rays. The radiative transfer of Ly$\alpha$ is implemented
in a simple approach that includes scattering by H I and absorption by
molecules and dust. Because of their non-radial propagation path, scattered
Ly$\alpha$ photons deposit their energy deeper in the disk atmosphere than the
radially propagating FUV continuum photons. We find that Ly$\alpha$ has a
significant impact on the thermal structure of the atmosphere. Photochemical
heating produced by scattered Ly$\alpha$ photons interacting with water vapor
and OH leads to a layer of hot (1500 - 2500 K) molecular gas. The temperature
in the layer is high enough to thermally excite the H$_2$ to vibrational levels
from which they can be fluoresced by Ly$\alpha$ to produce UV fluorescent H$_2$
emission. The resulting atmospheric structure may help explain the origin of UV
fluorescent H$_2$ that is commonly observed from classical T Tauri stars.
