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  1. D300 大学院環境学研究科
  2. D300a 雑誌掲載論文
  3. 学術雑誌

THE FORMATION OF CORES OF GIANT PLANETS AT CONVERGENCE ZONES OF PLANETARY MIGRATION

http://hdl.handle.net/2237/25522
http://hdl.handle.net/2237/25522
912ad4d1-83ba-4d82-a316-79e6f5e6b4b7
名前 / ファイル ライセンス アクション
Sirono_2016_ApJ_830_65.pdf Sirono_2016_ApJ_830_65.pdf (1.2 MB)
Item type 学術雑誌論文 / Journal Article(1)
公開日 2017-01-24
タイトル
タイトル THE FORMATION OF CORES OF GIANT PLANETS AT CONVERGENCE ZONES OF PLANETARY MIGRATION
言語 en
著者 Sirono, Sin-iti

× Sirono, Sin-iti

WEKO 69116

en Sirono, Sin-iti

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Katayama, Masahumi

× Katayama, Masahumi

WEKO 69117

en Katayama, Masahumi

Search repository
アクセス権
アクセス権 open access
アクセス権URI http://purl.org/coar/access_right/c_abf2
権利
言語 en
権利情報 © 2016. The American Astronomical Society
抄録
内容記述 The formation of solid cores in giant planets of mass $\sim 10\,{M}_{\oplus }$ is numerically simulated following the scenario of Sándor et al. In this scenario, there are two convergence zones, corresponding to the outer and inner edges of the dead zone, where the torque exerted on planetary embryos by the gas nebula is zero. At the outer edge of the dead zone, anticyclonic vortices accumulate infalling dust aggregates, and planetary embryos are continuously formed in this scenario. We performed N-body simulations and show that massive objects of $\simeq 10\,{M}_{\oplus }$ are formed in ~2.5 Myr, starting from the embryos. The largest object is formed at the inner convergence zone, although planetary embryos are placed at the outer convergence zone. This is due to the scattering of embryos from the outer to the inner convergence zone, and the shorter damping timescale of eccentricity at the inner convergence zone compared to the outer one. We varied the migration timescale due to the torque from gas by changing the gas surface density around the convergence zones. We found that there is a critical migration timescale below which $10\,{M}_{\oplus }$-sized objects are formed. Furthermore, we conducted simulations in which the gas surface density evolves according to viscous accretion. The largest object is also formed at the inner convergence zone irrespective of the strength of turbulence. Throughout the simulations, the location of the largest mass is the inner convergence zone. We confirmed that the formation timescale of a core of a Jovian planet can be explained in this scenario.
言語 en
内容記述タイプ Abstract
出版者
言語 en
出版者 IOP publishing
言語
言語 eng
資源タイプ
資源タイプresource http://purl.org/coar/resource_type/c_6501
タイプ journal article
出版タイプ
出版タイプ VoR
出版タイプResource http://purl.org/coar/version/c_970fb48d4fbd8a85
DOI
関連タイプ isVersionOf
識別子タイプ DOI
関連識別子 https://doi.org/10.3847/0004-637X/830/2/65
ISSN
収録物識別子タイプ PISSN
収録物識別子 0004-637X
書誌情報 en : Astrophysical Journal

巻 830, 号 2, p. 65-65, 発行日 2016-10-11
著者版フラグ
値 publisher
URI
識別子 http://doi.org/10.3847/0004-637X/830/2/65
識別子タイプ DOI
URI
識別子 http://hdl.handle.net/2237/25522
識別子タイプ HDL
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