Oral Presentation
Magnetic Fields in High-Mass Star Forming Region G10.62-0.38
Presenter: Benjamin Wu (NAOJ)
The role of magnetic fields in the high-mass star-forming (HMSF) process is a long-standing question. In particular, it is still undetermined what the relative strengths are between the most important mechanisms -- turbulence, gravity, and magnetic fields -- at core scales (~1000 AU), and if this balance is universal or variable. Utilizing ALMA’s new polarization capabilities, 29 HMSF regions containing >60 cores are currently being observed at ~500-1000 AU resolutions. Here, we present results of ALMA 250 GHz dust polarization observations of G10.62-0.38. These unprecedented observations detect over 100 independent polarization vectors, revealing well-ordered fields that are aligned parallel to the HMSF filament and in the direction of a clear velocity gradient -- but with notable deviations. We analyze the degree of turbulence, gravity, magnetic field orientation and inferred strength.
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