The Weakening Outburst of the Young Eruptive Star V582 Aur

Zsidi, G.; Ábrahám, P.; Acosta-Pulido, J. A.; Kóspál, Á.; Kun, M.; Szabó, Zs. M.; Bódi, A.; Cseh, B.; Castro Segura, N.; Hanyecz, O.; Ignácz, B.; Kalup, Cs.; Kriskovics, L.; Mészáros, L.; Ordasi, A.; Pál, A.; Sárneczky, K.; Seli, B.; Sódor, Á.; Szakáts, R.
Referencia bibliográfica

The Astrophysical Journal, Volume 873, Issue 2, article id. 130, 6 pp. (2019).

Fecha de publicación:
3
2019
Número de autores
20
Número de autores del IAC
1
Número de citas
7
Número de citas referidas
7
Descripción
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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