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We investigate the variability of the brightness distribution and thechanging density structure of the protoplanetary disk around DR Tau, aclassical T Tauri star. DR Tau is known for its peculiar variations from theultraviolet (UV) to the mid-infrared (MIR). Our goal is to constrain thetemporal variation of the disk structure based on photometric and MIRinterferometric data. We observed DR Tau with the MID-infrared Interferometricinstrument (MIDI) at the Very Large Telescope Interferometer (VLTI) at threeepochs separated by about nine years, two months, respectively. We fit thespectral energy distribution and the MIR visibilities with radiative transfersimulations. We are able to reproduce the spectral energy distribution as wellas the MIR visibility for one of the three epochs (third epoch) with a basicdisk model. We were able to reproduce the very different visibility curveobtained nine years earlier with a very similar baseline (first epoch), usingthe same disk model with a smaller scale height. The same density distributionalso reproduces the observation made with a higher spatial resolution in thesecond epoch, i.e. only two months before the third epoch.

DR Tau: Temporal variability of the brightness distribution in the potential planet-forming region