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Young stars are known to show variability due to non-steady mass accretionrate from their circumstellar disks. Accretion flares can produce strongenergetic irradiation and heating that may affect the disk in the planetformation region, close to the central star. During an extreme accretionoutburst in the young star EX Lupi, the prototype of EXor variables, remarkablechanges in molecular gas emission from $\sim1$ AU in the disk have recentlybeen observed (Banzatti et al. 2012). Here, we focus on water vapor and explorehow it is affected by variable accretion luminosity in T Tauri stars. Wemonitored a young highly variable solar-mass star, DR Tau, using simultaneouslytwo high/medium-resolution ESO-VLT spectrographs: VISIR at 12.4 $\mu$m toobserve water lines from the disk, and X-shooter covering from 0.3 to 2.5$\mu$m to constrain the stellar accretion. Three epochs spanning timescalesfrom several days to several weeks were obtained. Accretion luminosity wasestimated to change within a factor $\sim2$, and no change in water emissionwas detected at a significant level. In comparison to EX Lupi and EXoroutbursts, DR Tau suggests that the less long-lived and weaker variabilityphenomena typical of T Tauri stars may leave water at planet-forming radii inthe disk mostly unaffected. We propose that these systems may provide evidencefor two processes that act over different timescales: UV photochemistry in thedisk atmosphere (faster) and heating of the disk deeper layers (slower).

A UV-to-MIR monitoring of DR Tau: exploring how water vapor in the planet formation region of the disk is affected by stellar accretion variability