UJF-Grenoble 1/CNRS-INSU, Institut de Planétologie et d’Astrophysique de
Grenoble (IPAG) UMR 5274,
2 Crimean Astrophysical Observatory, Scientific Research institute, 98409 Nauchny, Crimea, Ukraine
3 Astronomical Institute Anton Pannekoek, Science Park 904, PO Box 94249, 1090 GE Amsterdam, The Netherlands
4 Centro de Astrobiologa (INTA-CSIC), PO Box 78, 28691 Villanueva de la Cañada, Spain
Accepted: 25 March 2013
Context. AA Tau has been monitored for more than 20 years since 1987 and exhibited a nearly constant brightness level of V = 12.5 mag. We report here that in 2011 it suddenly faded, becoming 2 mag fainter in the V-band, and has remained in this deep state since then.
Aims. We investigate the origin of the sudden dimming of the AA Tau system.
Methods. We report on new optical and near-IR photometry and spectroscopy obtained during the fading event.
Results. The system appears to be much redder and fainter than it was in the bright state. Moreover, the 8.2 d photometric period continuously observed for more than 20 years is not detected during most of the deep state. The analysis of the system’s brightness and colors suggests that the visual extinction on the line of sight has increased by about 3–4 mag in the deep state. At optical wavelengths, the system appears to be dominated by scattered light, probably originating from the upper surface layers of a highly inclined circumstellar disk. The profiles of the Balmer lines have significantly changed as well, with the disappearance of a central absorption component regularly observed in the bright state. We ascribe this change to the scattering of the system’s spectrum by circumstellar dust. Remarkably, the mass accretion rate in the inner disk and onto the central star has not changed as the system faded.
Conclusions. We conclude that the deepening of the AA Tau system is due to a sudden increase of circumstellar dust extinction on the line of sight without concomitant change in the accretion rate. We suggest that the enhanced obscuration may be produced by a nonaxisymmetric overdense region in the disk, located at a distance of 7.7 AU or more, that was recently brought into the line of sight by its Keplerian motion around the central star.
Key words: accretion, accretion disks / stars: individual: AA Tau / stars: pre-main sequence / stars: variables: T Tauri, Herbig Ae/Be
Based on observations made with telescopes at the Crimean Astrophysical Observatory, at the Calar Alto Observatory, and at ESO Paranal Observatory under programme ID 288.C-5026(A).
Photometric measurements are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (220.127.116.11) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/557/A77
© ESO, 2013