| Abstract
| - Aims.We aim to characterize the U-band variability of young brown dwarfs in the Taurus Molecular Cloud and discuss its origin. Methods.We used the XMM-Newton Extended Survey of the Taurus Molecular Cloud, where a sample of 11 young bona fide brown dwarfs (spectral type later than M 6) were observed simultaneously in X-rays with XMM-Newton and in the U-band with the XMM-Newton Optical/UV Monitor (OM). Results.We obtained upper limits to the U-band emission of 10 brown dwarfs ( U≥ 19.6-20.6 mag), whereas 2MASS J04141188+2811535 was detected in the U-band. Remarkably, the magnitude of this brown dwarf increased regularly from U ~ 19.5 mag at the beginning of the observation, peaked 6h later at U ~ 18.4 mag, and then decreased to U ~ 18.65 mag in the next 2 h. The first OM U-band measurement is consistent with the quiescent level observed about one year later thanks to ground follow-up observations. This brown dwarf was not detected in X-rays by XMM-Newton during the OM observation. Conclusions.We discuss the possible sources of U-band variability for this young brown dwarf, namely a magnetic flare, non-steady accretion onto the substellar surface, and rotational modulation of a hot spot. We conclude that this event is related to accretion from a circumsubstellar disk, where the mass accretion rate was about a factor of 3 higher than during the quiescent level.
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