3D radiative transfer of intrinsically polarized dust emission based on
  aligned aspherical grains
  (Sub-)Millimeter observations of the polarized emission of aligned aspherical
dust grains enable us to study the magnetic fields within protoplanetary disk.
However, the interpretation of these observations is complex. One must consider
the various effects that alter the measured polarized signal, such as the shape
of dust grains, the efficiency of grain alignment, the magnetic field
properties, and the projection of the signal along the line of sight. We aim at
analyzing observations of the polarized dust emission by disentangling the
effects on the polarization signal in the context of 3D radiative transfer
simulations. For this purpose, we developed a code capable of simulating dust
grain alignment of aspherical grains and intrinsical polarization of thermal
dust emission. We find that the influence of thermal polarization and dust
grain alignment on the polarized emission displayed as spatially resolved
polarization map or as spectral energy distribution trace disk properties which
are not traced in total (unpolarized) emission such as the magnetic field
topology. The radiative transfer simulations presented in this work enable the
3D analysis of intrinsically polarized dust emission - observed with, e.g.,
ALMA - which is essential to constrain magnetic field properties.
