Kavli Affiliate: David A. Principe
| First 5 Authors: Antonio S. Hales, Sebastián Pérez, Camilo Gonzalez-Ruilova, Lucas A. Cieza, Jonathan P. Williams
| Summary:
We present Atacama Large Millimeter/submillimeter Array (ALMA) 1.3 mm
observations of four young, eruptive star-disk systems at 0.4" resolution: two
FUors (V582 Aur and V900 Mon), one EXor (UZ Tau E) and one source with an
ambiguous FU/EXor classification (GM Cha). The disks around GM Cha, V900 Mon
and UZ Tau E are resolved. These observations increase the sample of FU/EXors
observed at sub-arcsecond resolution by 15%. The disk sizes and masses of
FU/EXors objects observed by ALMA so far suggest that FUor disks are more
massive than Class 0/I disks in Orion and Class II disks in Lupus of similar
size. EXor disks in contrast do not seem to be distinguishable from these two
populations. We reach similar conclusions when comparing the FU/EXor sample to
the Class I and Class II disks in Ophiuchus. FUor disks around binaries are
host to more compact disks than those in single-star systems, similar to
non-eruptive young disks. We detect a wide-angle outflow around GM Cha in
$^{12}$CO emission, wider than typical Class I objects and more similar to
those found around some FUor objects. We use radiative transfer models to fit
the continuum and line data of the well-studied disk around UZ Tau E. The line
data is well described by a keplerian disk, with no evidence of outflow
activity (similar to other EXors). The detection of wide-angle outflows in
FUors and not in EXors support to the current picture in which FUors are more
likely to represent an accretion burst in the protostellar phase (Class I),
while EXors are smaller accretion events in the protoplanetary (Class II)
phase.
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