  Lava planets have non-global, condensible atmospheres similar to icy bodies
within the solar system. Because they depend on interior dynamics, studying the
atmospheres of lava planets can lead to understanding unique geological
processes driven by their extreme environment. Models of lava planet
atmospheres have thus far focused on either radiative transfer or
hydrodynamics. In this study, we couple the two processes by introducing
ultraviolet and infrared radiation to a turbulent boundary layer model. We also
test the effect of different vertical temperature profiles on atmospheric
dynamics. Results from the model show that UV radiation affects the atmosphere
much more than IR. UV heating and cooling work together to produce a
horizontally isothermal atmosphere away from the sub-stellar point regardless
of the vertical temperature profile. We also find that stronger temperature
inversions induce stronger winds and hence cool the atmosphere. Our simulated
transmission spectra of the bound atmosphere show a strong SiO feature in the
UV that would be challenging to observe in the planet's transit spectrum due to
the precision required. Our simulated emission spectra are more promising, with
significant SiO spectral features at 4.5 and 9 $\mu$m that can be observed with
the James Webb Space Telescope. Different vertical temperature profiles produce
discernible dayside emission spectra, but not in the way one would expect.
