The Weakening Outburst of the Young Eruptive Star V582 Aur
Cseh, B.; Kriskovics, L.; Pál, A.; Ábrahám, P.; Kóspál, Á.; Szabó, Zs. M.; Kun, M.; Castro Segura, N.; Acosta-Pulido, J. A.; Sárneczky, K.; Sódor, Á.; Bódi, A.; Hanyecz, O.; Ignácz, B.; Ordasi, A.; Szakáts, R.; Zsidi, G.; Seli, B.; Kalup, Cs.; Mészáros, L.
Hungary, Spain, Germany, United Kingdom
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.