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Lava planets have non-global, condensible atmospheres similar to icy bodieswithin the solar system. Because they depend on interior dynamics, studying theatmospheres of lava planets can lead to understanding unique geologicalprocesses driven by their extreme environment. Models of lava planetatmospheres have thus far focused on either radiative transfer orhydrodynamics. In this study, we couple the two processes by introducingultraviolet and infrared radiation to a turbulent boundary layer model. We alsotest the effect of different vertical temperature profiles on atmosphericdynamics. Results from the model show that UV radiation affects the atmospheremuch more than IR. UV heating and cooling work together to produce ahorizontally isothermal atmosphere away from the sub-stellar point regardlessof the vertical temperature profile. We also find that stronger temperatureinversions induce stronger winds and hence cool the atmosphere. Our simulatedtransmission spectra of the bound atmosphere show a strong SiO feature in theUV that would be challenging to observe in the planet's transit spectrum due tothe precision required. Our simulated emission spectra are more promising, withsignificant SiO spectral features at 4.5 and 9 $\mu$m that can be observed withthe James Webb Space Telescope. Different vertical temperature profiles producediscernible dayside emission spectra, but not in the way one would expect.

The impact of ultraviolet heating and cooling on the dynamics and observability of lava planet atmospheres