CARATTI O GARATTI, AlessioAlessioCARATTI O GARATTIStecklum, B.B.StecklumGarcia Lopez, R.R.Garcia LopezEislöffel, J.J.EislöffelRay, T. P.T. P.RaySANNA, ALBERTOALBERTOSANNACESARONI, RiccardoRiccardoCESARONIWalmsley, C. M.C. M.WalmsleyOudmaijer, R. D.R. D.Oudmaijerde Wit, W. J.W. J.de WitMOSCADELLI, LucaLucaMOSCADELLIGreiner, J.J.GreinerKrabbe, A.A.KrabbeFischer, C.C.FischerKlein, R.R.KleinIbañez, J. M.J. M.Ibañez2021-02-192021-02-1920171745-2473http://hdl.handle.net/20.500.12386/30471Solar-mass stars form via disk-mediated accretion. Recent findings indicate that this process is probably episodic in the form of accretion bursts, possibly caused by disk fragmentation. Although it cannot be ruled out that high-mass young stellar objects arise from the coalescence of their low-mass brethren, the latest results suggest that they more likely form via disks. It follows that disk-mediated accretion bursts should occur. Here we report on the discovery of the first disk-mediated accretion burst from a roughly twenty-solar-mass high-mass young stellar object. Our near-infrared images show the brightening of the central source and its outflow cavities. Near-infrared spectroscopy reveals emission lines typical for accretion bursts in low-mass protostars, but orders of magnitude more luminous. Moreover, the released energy and the inferred mass-accretion rate are also orders of magnitude larger. Our results identify disk-accretion as the common mechanism of star formation across the entire stellar mass spectrum.STAMPAenArticle10.1038/nphys39422-s2.0-84995538621000395814000020http://arxiv.org/abs/1704.02628v1https://www.nature.com/articles/nphys39422017NatPh..13..276CFIS/05 - ASTRONOMIA E ASTROFISICA