 |
|
| EPoS 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 |