Planetesimal and planet formation in transient dust traps

被引:6
作者
Sandor, Zs. [1 ,2 ,3 ]
Guilera, O. M. [4 ,5 ,6 ]
Regaly, Zs. [2 ,3 ]
Lyra, W. [7 ]
机构
[1] Eotvos Lorand Univ, Inst Phys & Astron, Dept Astron, Pazmany Peter Setany 1-A, H-1117 Budapest, Hungary
[2] HUN REN Res Ctr Astron & Earth Sci, Konkoly Observ, Konkoly Thege Miklos Ut 15-17, H-1121 Budapest, Hungary
[3] MTA Ctr Excellence, CSFK, Konkoly Thege Miklos Ut 15-17, H-1121 Budapest, Hungary
[4] Natl Sci & Tech Res Council, Astrophys Inst La Plata, Paseo Bosque S-N, RA-1900 La Plata, Argentina
[5] Natl Univ La Plata, Paseo Bosque S-N, RA-1900 La Plata, Argentina
[6] Millennium Nucleus Planetary Format NPF, Valparaiso, Chile
[7] New Mexico State Univ, Dept Astron, POB 30001 MSC 4500, Las Cruces, NM 88001 USA
关键词
planets and satellites: formation; protoplanetary disks; planet-disk interactions; ISOTHERMAL GASEOUS DISK; PEBBLE ACCRETION; RAPID FORMATION; GIANT PLANETS; 3-DIMENSIONAL INTERACTION; STREAMING INSTABILITY; SHEAR INSTABILITY; GAS-GIANT; DEAD ZONE; PROTOPLANETARY;
D O I
10.1051/0004-6361/202347605
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Context. The ring-like structures in protoplanetary discs that are observed in the cold dust emission by ALMA might be explained by dust aggregates trapped aerodynamically in pressure maxima. Aims. We investigate the effect of a transient pressure maximum that develops between two regimes with different turbulent levels. We study how such a pressure maximum collects dust aggregates and transforms them into large planetesimals and Moon-mass cores that can further grow into a few Earth-mass planets by pebble accretion, and eventually into giant planets by accreting a gaseous envelope. Methods. We developed a numerical model, incorporating the evolution of a gaseous disc, the growth and transport of pebbles, N-body interactions of growing planetary cores, and their backreaction to a gas disc by opening a partial gap. Planetesimal formation by streaming instability is parametrised in our model. Results. A transient pressure maximum efficiently accumulates dust particles that can grow larger than millimetre-sized. If this happens, dust aggregates can be transformed by the streaming instability process into large planetesimals, which can grow further by pebble accretion according to our assumptions. As the gas evolves towards a steady state, the pressure maximum vanishes, and the concentrated pebbles not transformed into planetesimals and accreted by the growing planet drift inward. During this inward drift, if the conditions of the streaming instability are met, planetesimals are formed in the disc within a wide radial range. Conclusions. A transient pressure maximum is a favourable place for planetesimal and planet formation during its lifetime and the concentration of pebbles induces continuous formation of planetesimals even after its disappearance. In addition, the formation of a planet can trigger the formation of planetesimals over a wide area of the protoplanetary disc.
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页数:15
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