  V582 Aur is an FU Ori-type young eruptive star in outburst since $\sim$1985.
The eruption is currently in a relatively constant plateau phase, with
photometric and spectroscopic variability superimposed. Here we will
characterize the progenitor of the outbursting object, explore its environment,
and analyse the temporal evolution of the eruption. We are particularly
interested in the physical origin of the two deep photometric dips, one
occurred in 2012, and one is ongoing since 2016. We collected archival
photographic plates, and carried out new optical, infrared, and millimeter wave
photometric and spectroscopic observations between 2010 and 2017, with high
sampling rate during the current minimum. Beside analysing the color changes
during fading, we compiled multiepoch spectral energy distributions, and fitted
them with a simple accretion disk model. Based on pre-outburst data and a
millimeter continuum measurement, we suggest that the progenitor of the V582
Aur outburst is a low-mass T Tauri star with average properties. The mass of an
unresolved circumstellar structure, probably a disk, is 0.04 M$_{\odot}$. The
optical and near-infrared spectra demonstrate the presence of hydrogen and
metallic lines, show the CO bandhead in absorption, and exhibit a variable
H$\alpha$ profile. The color variations strongly indicate that both the $\sim$1
year long brightness dip in 2012, and the current minimum since 2016 are caused
by increased extinction along the line of sight. According to our accretion
disk models, the reddening changed from $A_V$=4.5 mag to 12.5 mag, while the
accretion rate remained practically constant. Similarly to the models of the
UXor phenomenon of intermediate and low-mass young stars, orbiting disk
structures could be responsible for the eclipses.
