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Measuring polarization from thermal dust emission can provide constraints onthe magnetic field structure around embedded protostars. However, interpretingthe observations is challenging without models that consistently account forboth the complexity of the protostellar birth environment and polarizationmechanisms. We aim to provide a better understanding with a focus onbridge-like structures such as that observed towards the protostellar multipleIRAS 16293--2422 by comparing synthetic polarization maps of thermal reemissionwith observations. We analyze the magnetic field properties associated with theformation of a protostellar multiple based on ideal MHD 3D zoom-in simulationscarried out with the RAMSES code. To compare with observations, we post-processa snapshot of a bridge-like structure that is associated with a forming triplestar system with the radiative transfer code POLARIS and producemulti-wavelength dust polarization maps. In the most prominent bridge of oursample, the typical density is about 10^(-16) g cm^(-3), and the magnetic fieldstrength is about 1 to 2 mG. The magnetic field structure has an elongatedtoroidal morphology and the dust polarization maps trace the complexmorphology. In contrast, the magnetic field strength associated with thelaunching of asymmetric bipolar outflows is significantly more magnetized (~100mG). At {\lambda}=1.3 mm, the orientation of grains in the bridge is similarfor the case accounting for radiative alignment torques (RATs) compared toperfect alignment with magnetic field lines. However, the polarization fractionin the bridge is three times smaller for the RAT scenario compared to assumingperfect alignment. At shorter wavelengths ({\lambda} < 200 {\mu}m), dustpolarization does not trace the magnetic field because other effects such asself-scattering and dichroic extinction dominate the orientation of thepolarization.

Linear dust polarization during the embedded phase of protostar formation