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New ALMA observations of protoplanetary disks allow us to probe planetformation in other systems, giving us new constraints on planet formationprocesses. Meanwhile, studies of our own Solar System rely on constraintsderived in a completely different way. However, it is still unclear whatfeatures the Solar System's disk could have produced during its gas phase. Byrunning 2D isothermal hydro-simulations and a dust evolution model, we derivesynthetic images at 1.3 mm wavelength using the radiative transfer codeRADMC3D. We find that the embedded multiple giant planets strongly perturb theradial gas velocities of the disk, creating traffic jams in the dust. Theyproduce over-densities different from the ones created by pressure traps andlocated away from the planets' positions in the disk. By deriving the images at1.3mm from these dust distributions, we show that the traffic jams, observablewith a high resolution, further blur the link between the number of gaps andrings in disks and the number of embedded planets. We additionally show that asystem of 3 compact giant planets does not automatically produce bright outerrings at large radii in the disk. This means that high resolution observationsof disks of various sizes are needed to distinguish between different giantplanet formation scenarios during the disk phase, where the giants form eitherin the outer regions of the disks or in the inner regions. Finally, we findthat, even when the dust temperature is determined self-consistently, the dustmasses derived observationally might be off by up to a factor of ten comparedto the dust contained in our simulations due to the creation of optically thickregions. Our study clearly shows that in addition to the constraints fromexoplanets and the Solar System, ALMA has the power to constrain differentstages of planet formation already during the first few million years.

Constraining giant planet formation with synthetic ALMA images of the Solar System's natal protoplanetary disk