Giant planet formation at the pressure maxima of protoplanetary disks II. A hybrid accretion scenario

GUILERA, OCTAVIO M.; ZSOLT SÁNDOR; MARÍA PAULA RONCO; VENTURINI, JULIA; MARCELO MIGUEL MILLER BERTOLAMI

ASTRONOMY AND ASTROPHYSICS

EDP SCIENCES S A

Lugar: Paris; Año: 2020

0004-6361

Context.Recent high-resolution observations of protoplanetary disks have revealed ring-like structures that can be associated topressure maxima. Pressure maxima are known to be dust collectors and planet migration traps. The great majority of planet formationworks are based either on the pebble accretion model or on the planetesimal accretion model. However, recent studies proposed thepossible formation of Jupiter by the hybrid accretion of pebbles and planetesimals.Aims.We aim to study the full process of planet formation consisting of dust evolution, planetesimal formation and planet growth ata pressure maximum in a protoplanetary disk.Methods.We compute, through numerical simulations, the gas and dust evolution in a protoplanetary disk, including dust growth,fragmentation, radial drift and particle accumulation at a pressure maximum. The pressure maximum appears due to an assumedviscosity transition at the water ice-line. We also consider the formation of planetesimals by streaming instability and the formationof a moon-size embryo that grows into a giant planet by the hybrid accretion of pebbles and planetesimals, all within the pressuremaximum.Results.We find that the pressure maximum is an efficient collector of dust drifting inwards. The condition of planetesimal formationby streaming instability is fulfilled due to the large amount of dust accumulated at the pressure bump. Then, a massive core is quicklyformed (in∼104yr) by the accretion of pebbles. After the pebble isolation mass is reached, the growth of the core slowly continuesby the accretion of planetesimals. The energy released by planetesimal accretion delays the onset of runaway gas accretion, allowinga gas giant to form after∼1 Myr of disk evolution. The pressure maximum also acts as a migration trap.Conclusions.Pressure maxima generated by a viscosity transition at the water ice-line are preferential locations for dust traps,planetesimal formation by streaming instability and planet migration traps. All these conditions allow the fast formation of a giantplanet by the hybrid accretion of pebbles and planetesimals.