High-mass stars play a significant role in the physical and chemical evolution of their immediate vicinities, by their powerful stellar wind, ultraviolet emission, and supernova explosion. Although a notable progress has been achieved in understanding the formation of low-mass stars, the physical mechanisms behind the formation of high-mass stars is still not well understood. As the molecular clouds consist of partially ionized gas and dust, the magnetic field has been found to be omnipresent 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 not entirely clear. Recently, because of its very high angular resolution, ALMA has opened an opportunity to study the magnetic field 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 targets observed in the survey of Magnetic fields in Massive star-forming Regions (MagMaR), that contains 30 targets in total. This region likely shows the formation of a binary system separated by ~1740 AU. The magnetic field lines threading this area are found to be deformed, resembling an "hourglass" morphology in northeast-southwest orientation 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. Based on the Davis-Chandrasekhar-Fermi method, we estimate the magnetic field strength in the plane-of-sky. We also estimate the mass-to-flux ratio, the turbulent to magnetic energy ratio and other physical parameters to understand the current star formation scenario in this region. We will present the preliminary results obtained from our study.
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