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しし座流星群の暗い流星分布計測
https://nagano-nct.repo.nii.ac.jp/records/111
https://nagano-nct.repo.nii.ac.jp/records/111383032d6-bec7-4ffd-90de-cc421cb7f7a8
| 名前 / ファイル | ライセンス | アクション |
|---|---|---|
KJ00004093400.pdf (1.1 MB)
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| Item type | Departmental Bulletin Paper(1) | |||||
|---|---|---|---|---|---|---|
| 公開日 | 2012-06-01 | |||||
| タイトル | ||||||
| タイトル | しし座流星群の暗い流星分布計測 | |||||
| タイトル | ||||||
| タイトル | Faint Meteor Search of Leonid, 2001-2003 | |||||
| 言語 | en | |||||
| 言語 | ||||||
| 言語 | jpn | |||||
| キーワード | ||||||
| 言語 | en | |||||
| 主題Scheme | Other | |||||
| 主題 | Leonids | |||||
| キーワード | ||||||
| 言語 | en | |||||
| 主題Scheme | Other | |||||
| 主題 | dust trail | |||||
| キーワード | ||||||
| 言語 | en | |||||
| 主題Scheme | Other | |||||
| 主題 | radiant | |||||
| キーワード | ||||||
| 言語 | en | |||||
| 主題Scheme | Other | |||||
| 主題 | faint meteor | |||||
| キーワード | ||||||
| 言語 | en | |||||
| 主題Scheme | Other | |||||
| 主題 | mass index | |||||
| 資源タイプ | ||||||
| 資源タイプ識別子 | http://purl.org/coar/resource_type/c_6501 | |||||
| 資源タイプ | departmental bulletin paper | |||||
| その他（別言語等）のタイトル | ||||||
| その他のタイトル | Faint Meteor Search of Leonid, 2001-2003 | |||||
| 著者 |
大西, 浩次
× 大西, 浩次 |
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| 著者別名 |
OHNISHI, Kouji
× OHNISHI, Kouji |
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| 抄録 | ||||||
| 内容記述タイプ | Abstract | |||||
| 内容記述 | McNaught and Asher (2001) predicted the Leonids Meteor Storm in 2001 due to the 4-rev (1866 yr.) and 9-rev (1699 yr) dust trails of the Leonids. To measure the flux and magnitude distribution of very faint meteors, we performed deep imaging telescopic observations with the cooled CCD camera toward the radiant points of the Leonids. We observed the Leonids meteor storm Nov.18 UT 2001, and succeeded to separate the radiant points due to the 4-rev and 9-rev dust trails (Yanagisawa et al. 2003, Torii et al. 2003) and we also succeeded to detect the faint meteors under 10 magnitudes (Kohama et al. 2003). The flux of faint meteors increases with the population index of 2.4, and the flux was obtained as (4.2±2.1)×10^<-4>km^<-2>s^<-1>(mag≦+12). We have found no apparent cutoff of the flux at brighter than～12 magnitude. The size of meteoroid of 10th magnitude meteor is a several tenth μm. Such small meteoroids are not the meteoroids of 4-rev (1866 yr.) and 9-rev (1699 yr) dust trails, because it is considered that they cannot return around the orbit of dust trail due to the solar radiation pressure. Thus we have to consider the new physical mechanism to create such small meteoroids. To established the property of faint meteor distribution, we also performed the deep imaging telescopic observation at the duration of the Leonids 2002 and 2003. This paper describes the detailed observation circumstances of Leonids 2001, 2002, and 2003 and the preliminary result of faint meteor distribution of Leonids. | |||||
| 書誌情報 |
長野工業高等専門学校紀要 en : Memoirs of Nagano National College of Technology 巻 38, p. 87-94, 発行日 2004-06-30 |
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| 出版者 | ||||||
| 出版者 | 長野工業高等専門学校 | |||||
| ISSN | ||||||
| 収録物識別子タイプ | ISSN | |||||
| 収録物識別子 | 0286-1909 | |||||
| 書誌レコードID | ||||||
| 収録物識別子タイプ | NCID | |||||
| 収録物識別子 | AN00179170 | |||||
| フォーマット | ||||||
| 内容記述タイプ | Other | |||||
| 内容記述 | application/pdf | |||||
| 著者版フラグ | ||||||
| 出版タイプ | VoR | |||||
| 出版タイプResource | http://purl.org/coar/version/c_970fb48d4fbd8a85 | |||||
