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%Context: {Previous studies have indicated that the 372.4 GHz groundtransition of ortho-H$_2$D$^+$ might be a powerful probe of Proto-PlanetaryDisks. The line could be especially suited for study of the disk mid-plane,where the bulk of the mass resides and where planet formation takes place.}%Aims: {Provide detailed theoretical predictions for the line intensity,profile and maps expected for representative disk models.} %Methods: {Wedetermine the physical and chemical structure of the disks from the modeldeveloped by Ceccarelli & Dominik (2005). The line emission is computed withthe new radiative transfer method developed recently by Elitzur & Asensio Ramos(2006).} %Results: {We present intensity maps convolved with the expected ALMAresolution, which delineate the origin of the H$_2$D$^+$ 372.4 GHz line. In thedisk inner regions, the line probes the conditions in the mid-plane out toradial distances of a few tens of AU, where Solar-like planetary systems mightform. In the disk outermost regions, the line originates from slightly abovethe mid-plane. When the disk is spatially resolved, the variation of lineprofile across the image provides important information about the velocityfield. Spectral profiles of the entire disk flux show a double peak shape atmost inclination angles.} %Conclusions: {Our study confirms that the 372.4 GHzH$_2$D$^+$ line provides powerful diagnostics of the mid-plane ofProto-Planetary Disks. Current submillimeter telescopes are capable ofobserving this line, though with some difficulties. The future ALMAinterferometer will have the sensitivity to observe and even spatially resolvethe H$_2$D$^+$ line emission.}

H$_2$D$^+$ line emission in Proto-Planetary Disks