The weakening outburst of the young eruptive star V582 Aur. (arXiv:1902.03673v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Zsidi_G/0/1/0/all/0/1">G. Zsidi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Abraham_P/0/1/0/all/0/1">P. &#xc1;brah&#xe1;m</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Acosta_Pulido_J/0/1/0/all/0/1">J. A. Acosta-Pulido</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kospal_A/0/1/0/all/0/1">&#xc1;. K&#xf3;sp&#xe1;l</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kun_M/0/1/0/all/0/1">M. Kun</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Szabo_Z/0/1/0/all/0/1">Zs. M. Szab&#xf3;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bodi_A/0/1/0/all/0/1">A. B&#xf3;di</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cseh_B/0/1/0/all/0/1">B. Cseh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Segura_N/0/1/0/all/0/1">N. Castro Segura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hanyecz_O/0/1/0/all/0/1">O. Hanyecz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ignacz_B/0/1/0/all/0/1">B. Ign&#xe1;cz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kalup_C/0/1/0/all/0/1">Cs. Kalup</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kriskovics_L/0/1/0/all/0/1">L. Kriskovics</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Meszaros_L/0/1/0/all/0/1">L. M&#xe9;sz&#xe1;ros</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ordasi_A/0/1/0/all/0/1">A. Ordasi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pal_A/0/1/0/all/0/1">A. P&#xe1;l</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sarneczky_K/0/1/0/all/0/1">K. S&#xe1;rneczky</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Seli_B/0/1/0/all/0/1">B. Seli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sodor_A/0/1/0/all/0/1">&#xc1;. S&#xf3;dor</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Szakats_R/0/1/0/all/0/1">R. Szak&#xe1;ts</a>

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$-$2019 February, as well as publicly
available mid-infrared WISE data. We found that the source shows a significant
optical$-$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, than
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 $sim$80 years.

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$-$2019 February, as well as publicly
available mid-infrared WISE data. We found that the source shows a significant
optical$-$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, than
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 $sim$80 years.

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