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We present our analysis of the magnetic field structures from 6000 au to 100au scales in the Class 0 protostar B335 inferred from our JCMT POL-2observations and the ALMA archival polarimetric data. To interpret theobservational results, we perform a series of (non-)ideal MHD simulations ofthe collapse of a rotating non-turbulent dense core, whose initial conditionsare adopted to be the same as observed in B335, and generate syntheticpolarization maps. The comparison of our JCMT and simulation results suggeststhat the magnetic field on a 6000 au scale in B335 is pinched and well alignedwith the bipolar outflow along the east-west direction. Among all oursimulations, the ALMA polarimetric results are best explained with weakmagnetic field models having an initial mass-to-flux ratio of 9.6. However, wefind that with the weak magnetic field, the rotational velocity on a 100 auscale and the disk size in our simulations are larger than the observationalestimates by a factor of several. An independent comparison of our simulationsand the gas kinematics in B335 observed with the SMA and ALMA favors strongmagnetic field models with an initial mass-to-flux ratio smaller than 4.8. Wediscuss two possibilities resulting in the different magnetic field strengthsinferred from the polarimetric and molecular-line observations, (1)overestimated rotational-to-gravitational energy in B335 and (2) additionalcontributions in the polarized intensity due to scattering on a 100 au scale.

astrophysical journal/the astrophysical journal

JCMT POL-2 and ALMA polarimetric observations of 6000-100 au scales in  the protostar B335: linking magnetic field and gas kinematics in observations  and MHD simulations