Poster Presentation

An Unified Model for Bipolar Outflows from Young Stars : Kinematic Structures in HH 30

Author(s): Tsung-Han Ai (Institute of Astronomy and Astrophysics, Academic Sinica), Chun-Fan Liu(Institute of Astronomy and Astrophysics, Academic Sinica), Hsien Shang(Institute of Astronomy and Astrophysics, Academic Sinica), Doug Johnstone(Institute of Astronomy and Astrophysics, Academic Sinica, Institute of Astronomy and Astrophysics, Academic Sinica), Ruben Krasnopolsky(Institute of Astronomy and Astrophysics, Academic Sinica)

Presenter: Tsung-Han Ai (Institute of Astronomy and Astrophysics, Academia Sinica)

We demonstrate how a magnetized wind bubble, as proposed in the unified wind model of Shang et al.(2023) is applied to the well-known edge-on protostellar system of HH 30 for interpreting the overall structure of its outflow lobes. We obtain radio (ALMA) and optical (HST) data from the archive to cover both high- and low-velocity components. Three primary structures can be distinguished based on the distribution of emission along the positional axis on transverse position-velocity diagrams, i.e., an extremely high-velocity wide-angle wind component with large line widths observed in the optical, a low-velocity magnetized ambient medium seen in 12CO, and a region of compressed wind intermediate both in velocity and location between the wind and ambient shocks observed in 12CO. The nested and mixed velocity structures expected in the framework of magnetized bubbles can explain the elongated area of compressed wind, which are the consequences of magnetic interplay inside the bubble.