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2021.10.25-2021.10.30

Oct 26 Tue 10:00~11:30  太陽系小天体セミナー / Solar System Minor Body Seminar zoom

Oct 27 Wed 15:30~17:00  NAOJ Science Colloquium      zoom

詳細は以下をご覧下さい

10月26日(火)

キャンパス:三鷹
セミナー名:太陽系小天体セミナー
定例・臨時の別:定例
日時:10月26日(火曜日)10時00分~11時30分
場所:zoom
講演者:古荘玲子

世話人の連絡先
 名前:渡部潤一

備考:テレビ会議またはスカイプによる参加も可

10月27日(水)

Seminar:NAOJ Science Colloquium
Regularly Scheduled/Sporadic:Every Wednesday
Date and time:2021 Oct 27, 15:30-17:00
Place:zoom
Speaker:Hiroshi Kobayashi
Affiliation:Nagoya University
Title:Rapid formation of Gas Giant Planets via Collisional Coagulation from Dust Grains to Planetary Cores
Abstract:Gas-giant planets, such as Jupiter, Saturn and massive exoplanets, were formed via the gas accretion onto the solid cores each with a mass of roughly ten Earth masses. However, rapid radial migration due to disk-planet interaction prevents the formation of such massive cores via planetesimal accretion. Comparably rapid core growth via pebble accretion requires very massive protoplanetary disks because most pebbles fall into the central star. Although planetesimal formation, planetary migration, and gas-giant core formation have been studied with much effort, the full evolution path from dust to planets are still uncertain. Here we report the result of full simulations for collisional evolution from dust to planets in a whole disk. Dust growth with realistic porosity allows the formation of icy planetesimals in the inner disk (> 10 au), while pebbles formed in the outer disk drift to the inner disk and there grow to planetesimals. The growth of those pebbles to planetesimals suppresses their radial drift and supplies small planetesimals sustainably in the vicinity of cores. This enables rapid formation of sufficiently massive planetary cores within 0.2-0.4 million years, prior to the planetary migration. Our models shows first gas giants form at 2-7 au in rather common protoplanetary disks, in agreement with the exoplanet and solar systems.

Facilitator
-Name:Akimasa Kataoka

Comment:English

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