Szegedi-Elek, E.E.Szegedi-ElekÁbrahám, P.P.ÁbrahámWyrzykowski, Ł.Ł.WyrzykowskiKun, M.M.KunKóspál, Á.Á.KóspálChen, L.L.ChenMarton, G.G.MartonMoór, A.A.MoórKiss, C.C.KissPál, A.A.PálSzabados, L.L.SzabadosVarga, J.J.VargaVarga-Verebélyi, E.E.Varga-VerebélyiAndreas, C.C.AndreasBachelet, E.E.BacheletBischoff, R.R.BischoffBódi, A.A.BódiBreedt, E.E.BreedtBurgaz, U.U.BurgazButterley, T.T.ButterleyCarrasco, J. M.J. M.CarrascoČepas, V.V.ČepasDamljanovic, G.G.DamljanovicGezer, I.I.GezerGodunova, V.V.GodunovaGromadzki, M.M.GromadzkiGurgul, A.A.GurgulHardy, L.L.HardyHildebrandt, F.F.HildebrandtHoffmann, S.S.HoffmannHundertmark, M.M.HundertmarkIhanec, N.N.IhanecJanulis, R.R.JanulisKalup, Cs.Cs.KalupKaczmarek, Z.Z.KaczmarekKönyves-Tóth, R.R.Könyves-TóthKrezinger, M.M.KrezingerKruszyńska, K.K.KruszyńskaLittlefair, S.S.LittlefairMaskoliūnas, M.M.MaskoliūnasMészáros, L.L.MészárosMikołajczyk, P.P.MikołajczykMugrauer, M.M.MugrauerNetzel, H.H.NetzelOrdasi, A.A.OrdasiPakštienė, E.E.PakštienėRybicki, K. A.K. A.RybickiSárneczky, K.K.SárneczkySeli, B.B.SeliSimon, A.A.SimonŠiškauskaitė, K.K.ŠiškauskaitėSódor, Á.Á.SódorSokolovsky, K. V.K. V.SokolovskyStenglein, W.W.StengleinStreet, R.R.StreetSzakáts, R.R.SzakátsTOMASELLA, LinaLinaTOMASELLATsapras, Y.Y.TsaprasVida, K.K.VidaZdanavičius, J.J.ZdanavičiusZieliński, M.M.ZielińskiZieliński, P.P.ZielińskiZiółkowska, O.O.Ziółkowska2025-02-202025-02-2020200004-637Xhttp://hdl.handle.net/20.500.12386/36109We present optical-infrared photometric and spectroscopic observations of Gaia 18dvy, located in the Cygnus OB3 association at a distance of 1.88 kpc. Gaia 18dvy was noted by the Gaia alerts system when its light curve exhibited a ≳4 mag rise in 2018-2019. The brightening was also observable at mid-infared wavelengths. The infrared colors of Gaia 18dvy became bluer as the outburst progressed. Its optical and near-infrared spectroscopic characteristics in the outburst phase are consistent with those of bona fide FU Orionis-type young eruptive stars. The progenitor of the outburst is probably a low-mass K-type star with an optical extinction of ˜3 mag. A radiative transfer modeling of the circumstellar structure, based on the quiescent spectral energy distribution, indicates a disk with a mass of 4 × 10<SUP>-3</SUP> M<SUB>⊙</SUB>. Our simple accretion disk modeling implies that the accretion rate had been exponentially increasing for more than 3 yr until mid-2019, when it reached a peak value of 6.9 × 10<SUP>-6</SUP> M<SUB>⊙</SUB> yr<SUP>-1</SUP>. In many respects, Gaia 18dvy is similar to the FU Ori-type object HBC 722.STAMPAenArticle10.3847/1538-4357/aba129https://iopscience.iop.org/article/10.3847/1538-4357/aba1292020ApJ...899..130SFIS/05 - ASTRONOMIA E ASTROFISICA