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We present high spectral resolution optical spectra of three youngintermediate mass stars, in all of which we spectrally resolve the 6300Angstrom [OI] emission line. Two of these have a double peaked line profile. Wefit these data with a simple model of the [OI] emission caused byphoto-dissociation of OH molecules in the upper layer of a circumstellar diskby stellar UV radiation and thus translate the Doppler broadened [OI] emissionprofile into an amount of emission as a function of distance from the centralstar. The resulting spectra are in agreement with the expected disk shapes asderived from their spectral energy distribution. We find evidence for shadowingby an inner rim in the disk surrounding HD101412 and see a flaring diskstructure in HD179218 while the [OI] spectrum of HD135344 is more complex. The[OI] emission starts for all three targets at velocities corresponding to theirdust sublimation radius and extends up to radii of 10 -- 90 AU. This shows thatthis method can be a valuable tool in the future investigation of circumstellardisks.

The Structure of Protoplanetary Disks Surrounding Three Young Intermediate Mass Stars. I. Resolving the disk rotation in the [OI] 6300 \AA line