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In protoplanetary disks, sufficiently massive planets excite pressure bumps,which can then be preferred locations for forming new planet cores. We discusshow this loop may affect the architecture of multi-planet systems, and compareour predictions with observation. Our main prediction is that low-mass planetsand giant planets can each be divided into two subpopulations with differentlevels of mass uniformity. Low-mass planets that can and cannot reach thepebble isolation mass (the minimum mass required to produce a pressure bump)develop into intra-similar "Super-Earths" and more diverse "Earths",respectively. Gas giants that do and do not accrete envelope quickly developinto intra-similar "Jupiters" and more diverse "Saturns", respectively.Super-Earths prefer to form long chains via repeated pressure-bump planetformation, while Jupiter formation is usually terminated at pairs or tripletsdue to dynamical instability. These predictions are broadly consistent withobservations. In particular, we discover a previously overlooked massuniformity dichotomy among the observed populations of both low-mass planets(Earths vs. Super-Earths) and gas giants (Saturns vs. Jupiters). For low-massplanets, planets well below the pebble isolation mass ($\lesssim 3M_\oplus$ or$\lesssim 1.5 R_\oplus$ for sun-like stars) show significantly higherintra-system pairwise mass difference than planets around the pebble isolationmass. For gas giants, the period ratios of intra-system pairs show a bimodaldistribution, which can be interpreted as two subpopulations with differentlevels of mass uniformity. These findings suggest that pressure-bump planetformation could be an important ingredient in shaping planetary architectures.

Earths are not Super-Earths, Saturns are not Jupiters: Imprints of pressure-bump planet formation on planetary architectures