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Mid-infrared spectroscopy is one of the few ways to observe the compositionof the terrestial planet forming zone, the inner few au, of proto-planetarydisks. The species currently detected in the disk atmosphere, for example CO,CO2, H2O and C2H2, are theoretically enough to constrain the C/O ratio in thedisk surface. However, thermo-chemical models have difficulties in reproducingthe full array of detected species in the mid-infrared simultaneously. In aneffort to get closer to the observed spectra, we have included waterUV-shielding as well as more efficient chemical heating into thermo-chemicalcode Dust And Lines. We find that both are required to match the observedemission spectrum. Efficient chemical heating, in addition to traditionalheating from UV photons, is necessary to elevate the temperature of the wateremitting layer to match the observed excitation temperature of water. We findthat water UV-shielding stops UV photons from reaching deep into the disk,cooling down the lower layers with higher column. These two effects create ahot emitting layer of water with a column of 1-10$\times 10^{18}$ cm$^{-2}$.This is only 1-10% of the water column above the dust $\tau=1$ surface atmid-infrared wavelengths in the models and represents <1% of the total watercolumn.

Water UV-shielding in the terrestrial planet-forming zone: Implications from water emission