  The majority of gas giants (planets of masses $\gtrsim10^2 M_\oplus$) are
found to reside at distances beyond $\sim1$ au from their host stars. Within 1
au, the planetary population is dominated by super-Earths of $2-20 M_\oplus$.
We show that this dichotomy between inner super-Earths and outer gas giants can
be naturally explained should they form in nearly inviscid disks. In laminar
disks, a planet can more easily repel disk gas away from its orbit. The
feedback torque from the pile-up of gas inside the planet's orbit slows down
and eventually halts migration. A pressure bump outside the planet's orbit
traps pebbles and solids, starving the core. Gas giants are born cold and stay
cold: more massive cores are preferentially formed at larger distances, and
they barely migrate under disk feedback. We demonstrate this using 2D
hydrodynamical simulations of disk-planet interaction lasting up to $10^5$
years: we track planet migration and pebble accretion until both come to an end
by disk feedback. Whether cores undergo runaway gas accretion to become gas
giants or not is determined by computing 1D gas accretion models. Our
simulations show that in an inviscid minimum mass solar nebula, gas giants do
not form inside $\sim$0.5 au, nor can they migrate there while the disk is
present. We also explore the dependence on disk mass, and find that gas giants
form further out in less massive disks.

Earth and Planetary Astrophysics