  The growth of a pebble accreting planetary core is stopped when reaching its
\textit{isolation mass} that is due to a pressure maximum emerging at the outer
edge of the gap opened in gas. This pressure maximum traps the inward drifting
pebbles stopping the accretion of solids onto the core. On the other hand, a
large amount of pebbles ($\sim 100M_\oplus$) should flow through the orbit of
the core until reaching its isolation mass. The efficiency of pebble accretion
increases if the core grows in a dust trap of the protoplanetary disc. Dust
traps are observed as ring-like structures by ALMA suggesting the existence of
global pressure maxima in discs that can also act as planet migration traps.
This work aims to reveal how large a planetary core can grow in such a pressure
maximum by pebble accretion. In our hydrodynamic simulations, pebbles are
treated as a pressureless fluid mutually coupled to the gas via drag force. Our
results show that in a global pressure maximum the pebble isolation mass for a
planetary core is significantly larger than in discs with power-law surface
density profile. An increased isolation mass shortens the formation time of
giant planets.
