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V582 Aur is an FU Ori-type young eruptive star in outburst since $\sim$1985.The eruption is currently in a relatively constant plateau phase, withphotometric and spectroscopic variability superimposed. Here we willcharacterize the progenitor of the outbursting object, explore its environment,and analyse the temporal evolution of the eruption. We are particularlyinterested in the physical origin of the two deep photometric dips, oneoccurred in 2012, and one is ongoing since 2016. We collected archivalphotographic plates, and carried out new optical, infrared, and millimeter wavephotometric and spectroscopic observations between 2010 and 2017, with highsampling rate during the current minimum. Beside analysing the color changesduring fading, we compiled multiepoch spectral energy distributions, and fittedthem with a simple accretion disk model. Based on pre-outburst data and amillimeter continuum measurement, we suggest that the progenitor of the V582Aur outburst is a low-mass T Tauri star with average properties. The mass of anunresolved circumstellar structure, probably a disk, is 0.04 M$_{\odot}$. Theoptical and near-infrared spectra demonstrate the presence of hydrogen andmetallic lines, show the CO bandhead in absorption, and exhibit a variableH$\alpha$ profile. The color variations strongly indicate that both the $\sim$1year long brightness dip in 2012, and the current minimum since 2016 are causedby increased extinction along the line of sight. According to our accretiondisk models, the reddening changed from $A_V$=4.5 mag to 12.5 mag, while theaccretion rate remained practically constant. Similarly to the models of theUXor phenomenon of intermediate and low-mass young stars, orbiting diskstructures could be responsible for the eclipses.

An UXor among FUors: extinction related brightness variations of the young eruptive star V582 Aur