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The origin of Uranus and Neptune has long been challenging to explain, due tothe large orbital distances from the Sun. After a planetary embryo has beenformed, the main accretion processes are likely pebble, gas and planetesimalaccretion. Previous studies of Uranus and Neptune formation typically don'tconsider all three processes; and furthermore, do not investigate how theformation of the outer planet impacts the inner planet. In this paper we studythe concurrent formation of Uranus and Neptune via both pebble, gas andplanetesimal accretion. We use a dust-evolution model to predict the size andmass flux of pebbles, and derive our own fit for gas accretion. We do notinclude migration, but consider a wide range of formation locations between 12and 40au. If the planetary embryos form at the same time and with the samemass, our formation model with an evolving dust population is unable to produceUranus and Neptune analogues. This is because the mass difference between theplanets and the H-He mass fractions become too high. However, if the outerplanetary embryo forms earlier and/or more massive than the inner embryo, thetwo planets do form in a few instances when the disk is metal-rich anddissipates after a few Myr. Furthermore, our study suggests that in-situformation is rather unlikely. Nethertheless, giant impacts and/or migrationcould potentially aid in the formation, and future studies including theseprocesses could bring us one step closer to understanding how Uranus andNeptune formed.

Can Uranus and Neptune form concurrently via pebble, gas and planetesimal accretion?