Resolving the FU Orionis System with ALMA: Interacting Twin Disks?

Simple item page
dc.contributor.authorPerez, Sebastian
dc.contributor.authorHales, Antonio
dc.contributor.authorLiu, Hauyu Baobab
dc.contributor.authorZhu, Zhaohuan
dc.contributor.authorCasassus, Simon
dc.contributor.authorWilliams, Jonathan
dc.contributor.authorZurlo, Alice
dc.contributor.authorCuello, Nicolas
dc.contributor.authorCieza, Lucas
dc.contributor.authorPrincipe, David
dc.date.accessioned2025-01-23T19:53:22Z
dc.date.available2025-01-23T19:53:22Z
dc.date.issued2020
dc.description.abstractFU Orionis objects are low-mass pre-main sequence stars characterized by dramatic outbursts several magnitudes in brightness. These outbursts are linked to episodic accretion events in which stars gain a significant portion of their mass. The physical processes behind these accretion events are not yet well understood. The archetypal FU Ori system, FU Orionis, is composed of two young stars with detected gas and dust emission. The continuum emitting regions have not been resolved until now. Here, we present 1.3 mm observations of the FU Ori binary system using the Atacama Large Millimeter/submillimeter Array. The disks are resolved at 40 mas resolution. Radiative transfer modeling shows that the emission from FU Ori north (primary) is consistent with a dust disk with a characteristic radius of similar to 11 au. The ratio between the major and minor axes shows that the inclination of the disk is similar to 37 degrees. FU Ori south is consistent with a dust disk of similar inclination and size. Assuming the binary orbit shares the same inclination angle as the disks, the deprojected distance between the north and south components is 06, i.e., similar to 250 au. Maps of (CO)-C-12 emission show a complex kinematic environment with signature disk rotation at the location of the northern component, and also (to a lesser extent) for FU Ori south. The revised disk geometry allows us to update FU Ori accretion models, yielding a stellar mass and mass accretion rate of FU Ori north of 0.6 M and 3.8 x 10(-5) M yr(-1), respectively.
dc.fuente.origenWOS
dc.identifier.doi10.3847/1538-4357/ab5c1b
dc.identifier.eissn1538-4357
dc.identifier.issn0004-637X
dc.identifier.urihttps://doi.org/10.3847/1538-4357/ab5c1b
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/100659
dc.identifier.wosidWOS:000520174700001
dc.issue.numero1
dc.language.isoen
dc.revistaAstrophysical journal
dc.rightsacceso restringido
dc.subjectStellar accretion disks
dc.subjectStar formation
dc.subjectFU Orionis stars
dc.subjectCircumstellar gas
dc.subjectSubmillimeter astronomy
dc.subjectMillimeter astronomy
dc.titleResolving the FU Orionis System with ALMA: Interacting Twin Disks?
dc.typeartículo
dc.volumen889
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
Files
Collections
Artículos de revistas