Poster Presentation
Unveiling the "hourglass" magnetic field in G333.46-0.16 using ALMA
Presenter: Piyali Saha (National Astronomical Observatory of Japan (NAOJ))
High-mass stars play a critical role in the physical and chemical evolution of their immediate surroundings, by their strong stellar wind, ultraviolet emission, and supernova explosion. Although significant progress has been made in understanding the formation of low-mass stars, the physical mechanisms behind the formation of high-mass stars is still under debate. As the molecular clouds consist of partially ionized gas and dust, the magnetic field has been found to be ubiquitous in the interstellar medium, and therefore, expected to affect the formation of low-mass as well as high-mass stars. However, the contribution of magnetic fields in the formation of high-mass stars is poorly understood. Recently, because of its very high angular resolution, ALMA has opened an opportunity to investigate the magnetic fields in the molecular clouds with minute details. We report the magnetic field geometry towards the high-mass star-forming region G333.46-0.16, which is obtained by ALMA at high-angular-resolution (~0.3") 1.2 millimeter observations. This is one of the sources observed in the survey of Magnetic fields in Massive star-forming Regions (MagMaR), that contains 30 targets in total. This region shows the formation of a binary system. The magnetic field lines threading this area are found to be deformed, acquiring an "hourglass" morphology on the plane-of-sky. Our aim is to investigate the interplay among turbulence, gravity, and magnetic field in the formation of stars at the core scale, and to find out the dominant agent between them. We will present the preliminary results obtained from our study.
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