Poster Presentation
Searching for Accretion Flows around Class 0 Protostars with ALMA
Presenter: Travis Thieme (NTHU)
As the envelope around a protostar collapses, a rotationally supported disk (RSD) forms due to conservation of angular momentum (e.g., Ulrich 1976). 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 (Li et al. 2014, Seifried et al. 2015). An increasing number of RSDs have been observed around the youngest Class 0 protostars (e.g., Murillo et al. 2013, Yen et al. 2017a). 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 (L1489-IRS: Yen et al. 2014; HL Tau: Yen et al. 2017b, 2019) and in one Class 0 source (VLA 1623: Cheong et al., submitted). 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: Ulrich 1976, Cassen & Moosman 1981).
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