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We present a detailed multi-wavelength characterization of the multi-ringdisk of HD 169142. We report new ALMA observations at 3 mm and analyze themtogether with archival 0.89 and 1.3 mm data. Our observations resolve three outof the four rings in the disk previously seen in high-resolution ALMA data. Asimple parametric model is used to estimate the radial profile of the dustoptical depth, temperature, density, and particle size distribution. We findthat the multiple ring features of the disk are produced by annularaccumulations of large particles, probably associated with gas pressure bumps.Our model indicates that the maximum dust grain size in the rings is $\sim1$cm, with slightly flatter power-law size distributions than the ISM-like sizedistribution ($p\sim3.5$) found in the gaps. In particular, the inner ring($\sim26$ au) is associated with a strong and narrow buildup of dust particlesthat could harbor the necessary conditions to trigger the streaminginstability. According to our analysis, the snowlines of the most importantvolatiles do not coincide with the observed substructures. We explore differentring formation mechanisms and find that planet-disk interactions are the mostlikely scenario to explain the main features of HD 169142. Overall, ourmulti-wavelength analysis provides some of the first unambiguous evidence ofthe presence of radial dust traps in the rings of HD 169142. A similar analysisin a larger sample of disks could provide key insights on the impact that disksubstructures have on the dust evolution and planet formation processes.

Characterization of Ring Substructures in the Protoplanetary Disk of HD 169142 from Multi-Wavelength ALMA Observations