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  1. B100 理学部/理学研究科
  2. B100a 雑誌掲載論文
  3. 学術雑誌

The Growth of Protoplanets via the Accretion of Small Bodies in Disks Perturbed by the Planetary Gravity

http://hdl.handle.net/2237/0002002042
http://hdl.handle.net/2237/0002002042
79b29503-fb83-46b3-a739-dd09be15e7c5
名前 / ファイル ライセンス アクション
Okamura_2021_ApJ_916_109.pdf Okamura_2021_ApJ_916_109.pdf (1.6 MB)
Item type itemtype_ver1(1)
公開日 2022-02-07
タイトル
タイトル The Growth of Protoplanets via the Accretion of Small Bodies in Disks Perturbed by the Planetary Gravity
言語 en
著者 Okamura, Tatsuya

× Okamura, Tatsuya

en Okamura, Tatsuya

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Kobayashi, Hiroshi

× Kobayashi, Hiroshi

en Kobayashi, Hiroshi

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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 © 2021. The American Astronomical Society
内容記述
内容記述 Planets grow via the collisional accretion of small bodies in a protoplanetary disk. Such small bodies feel strong gas drag, and their orbits are significantly affected by the gas flow and atmospheric structure around the planet. We investigate the gas flow in the protoplanetary disk perturbed by the gravity of the planet by 3D hydrodynamical simulation. We then calculate the orbital evolutions of particles in the gas structure obtained from the hydrodynamical simulation. Based on the orbital calculations, we obtain the collision rate between the planet and centimeter-to-kilometer-sized particles. Our results show that meter-sized or larger particles effectively collide with the planet owing to the atmospheric gas drag, which significantly enhances the collision rate. On the other hand, the gas flow plays an important role for smaller particles. Finally, considering the effects of the atmosphere and gas flow, we derive the new analytic formula for the collision rate, which is in good agreement with our simulations. We estimate the growth timescale and accretion efficiency of drifting bodies for the formation of a gas giant solid core using the formula. We find that the accretion of sub-kilometer-sized bodies achieves a short growth timescale (∼0.05 Myr) and a high accretion efficiency (∼1) for the core formation at 5 au in the minimum-mass solar nebula model.
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
関連情報
関連タイプ isVersionOf
識別子タイプ DOI
関連識別子 https://doi.org/10.3847/1538-4357/ac06c6
収録物識別子
収録物識別子タイプ PISSN
収録物識別子 0004-637X
書誌情報 en : The Astrophysical Journal

巻 916, 号 2, p. 109, 発行日 2021-08-04
ファイル公開日
日付 2022-02-07
日付タイプ Available
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