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アイテム
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Cometary dust modeling with aggregates consisting of submicron grains
https://jaxa.repo.nii.ac.jp/records/20548
https://jaxa.repo.nii.ac.jp/records/20548c37d558d-8a6c-42e5-8802-8ae9a65f7f3b
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 | Cometary dust modeling with aggregates consisting of submicron grains | |||||
言語 | ||||||
言語 | eng | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | 彗星ダスト | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | 星間物質 | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | 星間空間 | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | 光散乱 | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | 集合体 | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | 非晶質ケイ酸塩 | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | 有機質耐火性マントル | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | 赤外線スペクトル | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | 彗星 | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | cometary dust | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | interstellar matter | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | interstellar space | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | light scattering | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | aggregate | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | amorphous silicate | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | organic refractory mantle | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | infrared spectrum | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | comet | |||||
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 | |||||
著者 |
木村, 宏
× 木村, 宏× 千貝, 健× 山本, 哲生× Kimura, Hiroshi× Chigai, Takeshi× Yamamoto, Tetsuo |
|||||
著者所属 | ||||||
北海道大学低温科学研究所 | ||||||
著者所属 | ||||||
北海道大学低温科学研究所 | ||||||
著者所属 | ||||||
北海道大学低温科学研究所 | ||||||
著者所属(英) | ||||||
en | ||||||
Institute of Low Temperature Science, Hokkaido University | ||||||
著者所属(英) | ||||||
en | ||||||
Institute of Low Temperature Science, Hokkaido University | ||||||
著者所属(英) | ||||||
en | ||||||
Institute of Low Temperature Science, Hokkaido University | ||||||
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38回月・惑星シンポジウム en : Proceedings of the 38th ISAS Lunar and Planetary Symposium p. 123-123, 発行日 2006-03 |
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抄録(英) | ||||||
内容記述タイプ | Other | |||||
内容記述 | We model cometary dust by taking into account its formation and evolution. Light scattering, absorption, and emission properties of the dust expected from our model are compared with observations. We assume unprocessed cometary dust as primordial interstellar dust or agglomeration of the dust (Greenberg 1980; Yamamoto 1985). We use a model of Kimura et al. (2003a), in which interstellar dust is an aggregate consisting of submicron grains with an amorphous silicate core and an organic refractory mantle. Numerical and experimental simulations reveal that cluster-cluster aggregation processes take place in the early stages of particle growth. In such coagulation processes, dust is described as fractals with the fractal dimension D of approximately two. In the late stages, the fractal dimension increases and approaches D of approximately three. Therefore, unprocessed cometary dust is fractal aggregates of submicron grains having an amorphous silicate core and an organic refractory mantle. We also consider the possibility that explosive reactions of radicals in the organic refractory mantle crystallize amorphous silicates after ejection from cometary nuclei (Yamamoto & Chigai 2005). The wavelength and phase-angle dependences of intensity and linear polarization as well as the low albedo of cometary dust are correctly reproduced by our model as expected from the results in Kimura et al. (2003b). Infrared spectra of cometary dust are consistent with the hypothesis that long-period comets consist mainly of D of approximately two dust while short-period comets contain D of approximately three dust. We can even identify infrared silicate features with forsterite alone, inclusive of the feature that has been attributed to enstatite. More detailed results will be published elsewhere. | |||||
資料番号 | ||||||
内容記述タイプ | Other | |||||
内容記述 | 資料番号: AA0063350033 |