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The MPIA conference series
at Ringberg Castle
The MPIA conference series
at Ringberg Castle
 
EPoS 2020 Suggested Contribution
Searching for Accretion Flows around Class 0 Protostars with ALMA

Travis Thieme
NTHU, Hsinchu, TW
As the envelope around a protostar collapses, a rotationally supported disk (RSD) forms due to conservation of angular momentum. In more complicated scenarios, magneto-hydrodynamic (MHD) simulations show spiral-like streams of material (accretion flows) connecting the envelope to the disk in magnetized, turbulent cores. An increasing number of RSDs have been observed around the youngest Class 0 protostars. Understanding how material accretes to the disk from the envelope is important for describing the environments in which these disks are formed. These accretion flow structures have been reported in a few Class I protostars and in one Class 0 source. Our goal is to investigate ALMA archival data of Class 0 protostars with kinematic evidence of an RSD to look for extended accretion flow-like structures and compare their velocity structures to a simple infall model (CMU Model).
Caption: Possible accretion flows in two Class 0 protostars
Collaborators:
S. Lai, NTHU, TW
S. Lin, NTHU, TW
P. Cheung NTHU, TW
H. Yen, ASIAA, TW
D. Harsono, ASIAA, TW
Suggested Session: Cores2Disks