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The investigation of polarized light of protoplanetary disks is key forconstraining the dust properties, disk morphology and embedded magnetic fields.However, different polarization mechanisms and the diversity of dust grainshapes and compositions lead to ambiguities in the polarization pattern. Theso-called "self-scattering" of thermal, re-emitted radiation in the infraredand mm/submm is discussed as a major polarization mechanism. If the net flux ofthe radiation field is in radial direction, it is commonly assumed that thepolarization pattern produced by scattering in a protoplanetary disk showsconcentric rings for disks seen in face-on orientation. We show that a flip of$90^\circ$ of the polarization vectors may occur and mimic the typical patternof dichroic emission of dust grains aligned by a toroidal magnetic field indisks seen close to face-on. Furthermore, this effect of polarization reversalis a fast changing function of wavelength and grain size, and thus a powerfultool to constrain grain composition and size distribution present inprotoplanetary disks. In addition, the effect may also provide uniqueconstraints for the disk inclination, especially if the disk is seen close toface-on.

Polarization reversal of scattered thermal dust emission in protoplanetary disks at (sub-)mm wavelengths