Disk-mediated accretion burst in a high-mass young stellar object

DOI: 
10.1038/nphys3942
Publication date: 
01/03/2017
Main author: 
Caratti O Garatti A.
IAA authors: 
Ibañez, J.M.
Authors: 
Caratti O Garatti A., Stecklum B., Garcia Lopez R., Eislöffel J., Ray T.P., Sanna A., Cesaroni R., Walmsley C.M., Oudmaijer R.D., De Wit W.J., Moscadelli L., Greiner J., Krabbe A., Fischer C., Klein R., Ibañez J.M.
Journal: 
Nature Physics
Refereed: 
Yes
Publication type: 
Article
Volume: 
13
Pages: 
276-279
Abstract: 

Solar-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. © 2017 Macmillan Publishers Limited.

Database: 
ADS
SCOPUS
URL: 
https://www.scopus.com/inward/record.uri?eid=2-s2.0-84995538621&doi=10.1038%2fnphys3942&partnerID=40&md5=a6064c6db48b55499ef1a0710ceb41ca
ADS Bibcode: 
2017NatPh..13..276C