  Recent observations of protoplanetary disks have revealed ring-like
structures that can be associated to pressure maxima. Pressure maxima are known
to be dust collectors and planet migration traps. Most of planet formation
works are based either on the pebble accretion model or on the planetesimal
accretion model. However, recent studies proposed the possible formation of
Jupiter by the hybrid accretion of pebbles and planetesimals. We aim to study
the full process of planet formation consisting of dust evolution, planetesimal
formation and planet growth at a pressure maximum in a protoplanetary disk. We
compute, through numerical simulations, the gas and dust evolution, including
dust growth, fragmentation, radial drift and particle accumulation at a
pressure bump. We also consider the formation of planetesimals by streaming
instability and the formation of a moon-size embryo that grows into a giant
planet by the hybrid accretion of pebbles and planetesimals. We find that
pressure maxima in protoplanetary disks are efficient collectors of dust
drifting inwards. The condition of planetesimal formation by streaming
instability is fulfilled due to the large amount of dust accumulated at the
pressure bump. Then, a massive core is quickly formed (in $\sim 10^4$ yr) by
the accretion of pebbles. After the pebble isolation mass is reached, the
growth of the core slowly continues by the accretion of planetesimals. The
energy released by planetesimal accretion delays the onset of runaway gas
accretion, allowing a gas giant to form after $\sim$1 Myr of disk evolution.
The pressure maximum also acts as a migration trap. Pressure maxima in
protoplanetary disks are preferential locations for dust traps, planetesimal
formation by streaming instability and planet migration traps. All these
conditions allow the fast formation of a giant planet by the hybrid accretion
of pebbles and planetesimals.
