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Giant planets migrate though the protoplanetary disc as they grow. Weinvestigate how the formation of planetary systems depends on the radial fluxof pebbles through the protoplanetary disc and on the planet migration rate.Our N-body simulations confirm previous findings that Jupiter-like planets inorbits outside the water ice line originate from embryos starting out at 20-40AU when using nominal type-I and type-II migration rates and a pebble flux of100-200 Earth masses per million years, enough to grow Jupiter within thelifetime of the solar nebula. The planetary embryos placed up to 30AU migrateinto the inner system (r<1AU) and form super-Earths or hot and warm gas giants,producing systems that are inconsistent with the configuration of the solarsystem, but consistent with some exoplanetary systems. We also explore slowermigration rates which allow the formation of gas giants from embryosoriginating from the 5-10AU region, which are stranded exterior to 1 AU at theend of the gas-disc phase. We identify a pebble flux threshold below whichmigration dominates and moves the planetary core to the inner disc, where thepebble isolation mass is too low for the planet to accrete gas efficiently.Giant planet growth requires a sufficiently-high pebble flux to enable growthto out-compete migration. Even higher pebble fluxes produce systems withmultiple gas giants. We show that planetary embryos starting interior to 5AU donot grow into gas giants, even if migration is slow and the pebble flux islarge. Instead they grow to the mass regime of super-Earths. This stuntedgrowth is caused by the low pebble isolation mass in the inner disc and isindependent of the pebble flux. Additionally we show that the long termevolution of our formed planetary systems can produce systems with hotsuper-Earths and outer gas giants as well as systems of giants on eccentricorbits (abridged).

Formation of planetary systems by pebble accretion and migration: Growth of gas giants