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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

Coagulation Instability in Protoplanetary Disks: A Novel Mechanism Connecting Collisional Growth and Hydrodynamical Clumping of Dust Particles

http://hdl.handle.net/2237/0002002694
http://hdl.handle.net/2237/0002002694
1d35038d-fdc0-449f-b9a5-a2e867cb9a0c
名前 / ファイル ライセンス アクション
Tominaga_2021_ApJ_923_34.pdf Tominaga_2021_ApJ_923_34.pdf (2.1 MB)
Item type itemtype_ver1(1)
公開日 2022-05-10
タイトル
タイトル Coagulation Instability in Protoplanetary Disks: A Novel Mechanism Connecting Collisional Growth and Hydrodynamical Clumping of Dust Particles
言語 en
著者 Tominaga, Ryosuke T.

× Tominaga, Ryosuke T.

en Tominaga, Ryosuke T.

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Inutsuka, Shu-ichiro

× Inutsuka, Shu-ichiro

en Inutsuka, Shu-ichiro

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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 We present a new instability driven by a combination of coagulation and radial drift of dust particles. We refer to this instability as "coagulation instability" and regard it as a promising mechanism to concentrate dust particles and assist planetesimal formation in the very early stages of disk evolution. Because of dust-density dependence of collisional coagulation efficiency, dust particles efficiently (inefficiently) grow in a region of positive (negative) dust density perturbations, leading to a small radial variation of dust sizes and as a result radial velocity perturbations. The resultant velocity perturbations lead to dust concentration and amplify dust density perturbations. This positive feedback makes a disk unstable. The growth timescale of coagulation instability is a few tens of orbital periods even when dust-to-gas mass ratio is on the order of 10^−3. In a protoplanetary disk, radial drift and coagulation of dust particles tend to result in dust depletion. The present instability locally concentrates dust particles even in such a dust-depleted region. The resulting concentration provides preferable sites for dust–gas instabilities to develop, which leads to further concentration. Dust diffusion and aerodynamical feedback tend to stabilize short-wavelength modes, but do not completely suppress the growth of coagulation instability. Therefore, coagulation instability is expected to play an important role in setting up the next stage for other instabilities, such as streaming instability or secular gravitational instability, to further develop toward planetesimal formation.
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/ac173a
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 923, 号 1, p. 34, 発行日 2021-12-10
ファイル公開日
日付 2022-05-10
日付タイプ Available
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