We present mocassin 2D photoionisation and dust radiative transfer models of a prototypical T Tauri disk irradiated by X-rays from the young pre-main sequence star .
The calculations demonstrate a layer of hot gas reaching temperatures of \sim 10 ^ { 6 } K at small radii and \sim 10 ^ { 4 } K at a distance of 1 AU .
The gas temperatures decrease sharply with depth , but appear to be completely decoupled from dust temperatures down to a column depth of \sim 5 \times 10 ^ { 21 } cm ^ { -2 } .

We predict that several fine-structure and forbidden lines of heavy elements , as well as recombination lines of hydrogen and helium , should be observable with current and future instrumentation , although optical lines may be smothered by the stellar spectrum .
Predicted line luminosities are given for the the brightest collisionally excited lines ( down to \sim 10 ^ { -8 } L _ { \odot } ) , and for recombination transitions from several levels of H i and He i .

The mass loss rate due to X-ray photoevaporation estimated from our models is of the order of 10 ^ { -8 } M _ { \odot } yr ^ { -1 } , implying a dispersal timescale of a few Myr for a disk of mass 0.027 M _ { \odot } , which is the mass of the disk structure model we employed .
We discuss the limitations of our model and highlight the need for further calculations that should include the simultaneous solution of the 2D radiative transfer problem and the 1D hydrostatic equilibrium in the polar direction .