Effects of grain magnetic properties and grain growth on synthetic dust polarization of MHD simulations of low-mass Class 0/I YSOs

Thermal dust polarization is a powerful tool to probe magnetic fields (B) and grain properties. However, a systematic study of the dependence of dust polarization on grain properties in protostellar environments is not yet available. In this paper, we post-process a non-ideal MHD simulation of a collapsing protostellar core with our updated POLARIS code to study in detail the effects of iron inclusions and grain growth on thermal dust polarization. We found that superparamagnetic (SPM) grains can produce high polarization degree of p similar to 10-40 beyond similar to 500 au from the protostar because of their efficient alignment by magnetically enhanced radiative torque mechanism. The magnetic field turbulence in the envelope causes the decrease in p with increasing emission intensity I as p proportional to I-alpha with the slope alpha similar to -0.3. But within 500 au, SPM grains tend to have inefficient internal alignment and be aligned with {B} by RATs only, producing lower p similar to 1 and a steeper slope of alpha similar to -0.6. For paramagnetic (PM) grains, the alignment loss of grains above alpha similar to-0.9 in the inner similar to 200 au produces p<<1 and the polarization hole with alpha similar to -0.9. Grain growth can increase p in the envelope for SPM grains, but cause stronger depolarization for SPM grains in the inner similar to 500 au and for PM grains in the entire protostellar core. Finally, we found the increase of polarization angle dispersion function S with iron inclusions and grain growth, implying the dependence of B-field strength measured using the David-Chandrasekhar-Fermi technique on grain alignment and grain properties.