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The effect of imperfect sticking on the collisional growth of dust in the Jovian subnebula
https://jaxa.repo.nii.ac.jp/records/20595
https://jaxa.repo.nii.ac.jp/records/205956cf5d538-f199-4c16-b476-d595d50ffb5b
Item type | 会議発表論文 / Conference Paper(1) | |||||
---|---|---|---|---|---|---|
公開日 | 2015-03-26 | |||||
タイトル | ||||||
言語 | en | |||||
タイトル | The effect of imperfect sticking on the collisional growth of dust in the Jovian subnebula | |||||
言語 | ||||||
言語 | eng | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | 衝突成長 | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | 衛星形成 | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | 太陽星雲 | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | 木星 | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | 気体密度 | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | 質量密度 | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | 数値解析 | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | 模型 | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | collisional growth | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | satellite formation | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | solar nebula | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | Jupiter | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | gas density | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | mass density | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | numerical analysis | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | model | |||||
資源タイプ | ||||||
資源タイプ識別子 | http://purl.org/coar/resource_type/c_5794 | |||||
資源タイプ | conference paper | |||||
アクセス権 | ||||||
アクセス権 | metadata only access | |||||
アクセス権URI | http://purl.org/coar/access_right/c_14cb | |||||
その他のタイトル | ||||||
その他のタイトル | 木星のサブネビュラにおけるダストの衝突成長に対する不完全固着の影響 | |||||
著者 |
福井, 隆
× 福井, 隆× 島沢, 竜平× 倉本, 圭× Fukui, Takashi× Shimazawa, Ryuhei× Kuramoto, Kiyoshi |
|||||
著者所属 | ||||||
北海道大学 大学院理学研究科 | ||||||
著者所属 | ||||||
インテック | ||||||
著者所属 | ||||||
北海道大学 大学院理学研究科 | ||||||
著者所属(英) | ||||||
en | ||||||
Hokkaido University Graduate School of Science | ||||||
著者所属(英) | ||||||
en | ||||||
INTEC Inc. | ||||||
著者所属(英) | ||||||
en | ||||||
Hokkaido University Graduate School of Science | ||||||
出版者 | ||||||
出版者 | 宇宙航空研究開発機構宇宙科学研究本部 | |||||
出版者(英) | ||||||
出版者 | Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA/ISAS) | |||||
書誌情報 |
第37回月・惑星シンポジウム en : Proceedings of the 37th ISAS Lunar and Planetary Symposium p. 65-68, 発行日 2004-02 |
|||||
抄録(英) | ||||||
内容記述タイプ | Other | |||||
内容記述 | The Galilean satellites are considered to have been formed in the Jovian subnebula, which was produced during the gas capture of proto-Jupiter, according to the similar scenario to the planet formation in the solar nebula. However, it is not well understood whether or not all of elementary steps of the satellite formation are described by the scaled-down planet formation processes because the subnebula is so different from the solar nebula in temperature, density, time scale, and so on. In this study, concerned is the collisional growth of dust, the first stage of the satellite formation. During the growth due to mutual collisions, the dust particles fall toward Jupiter due to gas drag. Falling velocity strongly depends on the size of dust particles, and the particles with radius of 10(exp -2) to 1 m fall fastest. For a minimum mass Jovian subnebula model (Mosqueira and Estrada, 2003), the maximum falling velocity is about 120 m/s at the present orbit of Ganymede. At this velocity, a dust particle would reach Jupiter in three months. To form satellitesimals, it is necessary that the time scale of dust growth through this dangerous size range is shorter than that of falling. The time scale of collisional growth is estimated by performing a numerical computation taking it into account that dust particles can not stick when they collide in a very high velocity. Given is 10 m/s as the critical velocity for sticking (Dominik and Tielens, 1996). As a result, obtained is about one month as a minimum growth time. This indicates that the formation of satellitesimals is difficult without considering the effect of the formation of dust concentrated region or (and) the mechanism to increase the critical velocity to form satellitesimals. | |||||
資料番号 | ||||||
内容記述タイプ | Other | |||||
内容記述 | 資料番号: AA0047898017 |