期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 477, 期 1, 页码 593-615出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/sty569
关键词
planets and satellites: composition; planets and satellites: formation; planets and satellites: gaseous planets; planet-disc interactions; protoplanetary discs; brown dwarfs
资金
- STFC [ST/K001000/1, ST/N504117/1]
- ALICE High Performance Computing Facility at the University of Leicester
- STFC DiRAC HPC Facility [ST/H00856X/1, ST/K000373/1]
- STFC [ST/K001000/1, ST/M006948/1, ST/H00856X/1, PP/E00119X/1, ST/R002363/1, 1794975, ST/N000757/1, ST/H002235/1, ST/P002307/1] Funding Source: UKRI
We run numerical simulations to study the accretion of gas and dust grains on to gas giant planets embedded into massive protoplanetary discs. The outcome is found to depend on the disc cooling rate, planet mass, grain size, and irradiative feedback from the planet. If radiative cooling is efficient, planets accrete both gas and pebbles rapidly, open a gap, and usually become massive brown dwarfs. In the inefficient cooling case, gas is too hot to accrete on to the planet but pebble accretion continues and the planets migrate inward rapidly. Radiative feedback from the planet tends to suppress gas accretion. Our simulations predict that metal enrichment of planets by dust grain accretion inversely correlates with the final planet mass, in accordance with the observed trend in the inferred bulk composition of Solar system and exosolar giant planets. To account for observations, however, as many as similar to 30-50 per cent of the dust mass should be in the form of large grains.
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