Zsidi, G., Abraham, P., Acosta-Pulido, J.A., Kospal, A., Kun, M., Szabo, Zs. M., Bodi, A., Cseh, B., Castro Segura, N., Hanyecz, O., Ignacz, B., Kalup, Cs., Kriskovics, L., Meszaros, L., Ordasi, A., Pal, A., Sarneczky, K., Seli, B., Sodor, A. and Szakats, R. (2019) The weakening outburst of the young eruptive star V582 Aur. The Astrophysical Journal, 873, [130]. (doi:10.3847/1538-4357/ab05c9).
Abstract
V582 Aur is a pre-main-sequence FU Orionis type eruptive star, which entered a brightness minimum in 2016 March due to changes in the line-of-sight extinction. Here, we present and analyze new optical B, V, R C , and I C band multiepoch observations and new near-infrared J, H, and K S band photometric measurements from 2018 January–2019 February, as well as publicly available midinfrared Wide-field Infrared Survey Explorer (WISE) data. We found that the source shows a significant optical–near-infrared variability, and the current brightness minimum has not completely finished yet. If the present dimming originates from the same orbiting dust clump that caused a similar brightness variation in 2012, then our results suggest a viscous spreading of the dust particles along the orbit. Another scenario is that the current minimum is caused by a dust structure, that is entering and leaving the inner part of the system. The WISE measurements could be consistent with this scenario. Our long-term data, as well as an accretion disk modeling hint at a general fading of V582 Aur, suggesting that the source will reach the quiescent level in ~80 yr.
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