To study the transportation of magnetic flux from large to small scales in protostellar sources, we analyzed the Nobeyama 45m N2H+ (1-0), JCMT 850 um polarization, and ALMA C18O (2-1) and 1.3 and 0.8 mm (polarized) continuum data of the Class 0 protostar HH 211. The magnetic field strength in the dense core on a 0.1 pc scale was estimated with the single-dish line and polarization data using the DCF method, and that in the protostellar envelope on a 600 au scale was estimated from the force balance between the gravity and magnetic field tension by analyzing the gas kinematics and magnetic field structures with the ALMA data. Our analysis suggests that from 0.1 pc-600 au scales, the magnetic field strength increases from 40-107 uG to 0.3-1.2 mG, and the mass-to-flux ratio increases from 1.2-3.7 to 9.1-32.3. The increase in the mass-to-flux ratio could suggest that the magnetic field is partially decoupled from the neutral matter between 0.1 pc and 600 au scales, and hint at efficient ambipolar diffusion in the infalling protostellar envelope in HH 211.
[Poster PDF File]