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Dust coagulation in a protoplanetary disk is the first step of planetesimalformation. However, a pathway from dust aggregates to planetesimals remainsunclear. Both numerical simulations and laboratory experiments have suggestedthe importance of dust structure in planetesimal formation, but it is not wellconstrained by observations. We study how dust structure and porosity alterspolarimetric images at millimeter wavelength by performing 3D radiativetransfer simulations. Aggregates with different porosity and fractal dimensionare considered. As a result, we find that dust aggregates with lower porosityand/or higher fractal dimension are favorable to explain observedmillimeter-wave scattering polarization of disks. Aggregates with extremelyhigh porosity fail to explain the observations. In addition, we also show thatparticles with moderate porosity show weak wavelength dependence of scatteringpolarization, indicating that multi-wavelength polarimetry is useful toconstrain dust porosity. Finally, we discuss implications for dust evolutionand planetesimal formation in disks.

Unveiling Dust Aggregate Structure in Protoplanetary Disks by Millimeter-wave Scattering Polarization