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We present an integrated thermal-chemical model for the atmosphere of theinner region of a protoplanetary disk that includes irradiation by both farultraviolet (FUV) and X-ray radiation. We focus on how the photodissociation ofwater and OH affects the abundances of these and related species and how itcontributes to the heating of the atmosphere. The dust in the atmosphere playsseveral important roles, primarily as the site of H$_2$ formation and byabsorbing the FUV. Large amounts of water can be synthesized within the inner 4AU of a disk around a typical classical T~Tauri star. OH is found primarily atthe top of a warm region where the gas temperature is $T_g \approx 650 - 1000$K and water below it where the temperature is lower, $T_g \approx 250 - 650$ K.The amounts of water and OH and the temperatures of the regions in which theyformed are in agreement with recent Spitzer measurements and support the notionof it in situ production of water in the inner regions of protoplanetary disks.We find that the synthesized water is effective in shielding the disk midplanefrom stellar FUV radiation.

Shielding by Water and OH in FUV and X-ray Irradiated Protoplanetary Disks