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30cm 望遠鏡による太陽粒状斑の観測
https://jaxa.repo.nii.ac.jp/records/32811
https://jaxa.repo.nii.ac.jp/records/328118d0cea18-fadd-44ac-8160-3b2a30715d3b
名前 / ファイル | ライセンス | アクション |
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SA0166572.pdf (841.2 kB)
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Item type | 紀要論文 / Departmental Bulletin Paper(1) | |||||
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公開日 | 2015-03-26 | |||||
タイトル | ||||||
タイトル | 30cm 望遠鏡による太陽粒状斑の観測 | |||||
言語 | ||||||
言語 | jpn | |||||
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 | |||||
その他のタイトル(英) | ||||||
その他のタイトル | The Observation of Solar Granulation with a 30cm Balloon-Borne Telescope | |||||
著者 |
平山, 淳
× 平山, 淳× 浜名, 茂男× 徳家, 厚× 今井, 英樹× 清水, 一郎× 守山, 史生× 吉田, 安徳× 佐下橋, 市太郎× 丹羽, 登× HIRAYAMA, Tadashi× HAMANA, Shigeo× TOKUYA, Atsushi× IMAI, Hideki× SHIMIZU, Ichiro× MORIYAMA, Fumio× YOSHIDA, Yasunori× SAGEHASHI, Ichitaro× NIWA, Noboru |
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著者所属 | ||||||
東京大学東京天文台 | ||||||
著者所属 | ||||||
東京大学東京天文台 | ||||||
著者所属 | ||||||
東京大学東京天文台 | ||||||
著者所属 | ||||||
東京大学東京天文台 | ||||||
著者所属 | ||||||
東京大学東京天文台 | ||||||
著者所属 | ||||||
東京大学東京天文台 | ||||||
著者所属 | ||||||
宇宙開発事業団 | ||||||
著者所属 | ||||||
東京大学工学部境界領域研究施設 | ||||||
著者所属 | ||||||
千葉工業大学電気工学科 | ||||||
出版者 | ||||||
出版者 | 宇宙科学研究所 | |||||
出版者(英) | ||||||
出版者 | Institute of Space and Astronautical Science | |||||
書誌情報 |
宇宙科学研究所報告. 特集: 大気球研究報告 巻 4, p. 93-105, 発行日 1982-08 |
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抄録(英) | ||||||
内容記述タイプ | Other | |||||
内容記述 | Direct photographs of the solar granulation near the limb were obtained with a 30cm balloon-borne telescope. The observed position on the solar disk was at cosθ=0.7,where θ is the angle between the observer and the normal to the solar surface and the wavelength used was 545nm with a pass band of 40nm. Total half-width (FWHM) of the autocorrelation function of the contrast of the granulation was found to be 780km and 660km in radial and tangential direction to the solar limb, respectively. Although the latter value agrees with the older determination at the disk center, the distance, 2000km, to the minimum value of the auto-correlation function was much larger than those obtained by Leighton at the disk center. Two dimensional power spectrum was obtained and after corrections due to noise spectrum and finite resolution of the optical system, the root-mean-square brightness fluctuation of the granulation was found to be 7.0-7.9%. It is to be noted that the modulation transfer function of the optical system was determined at the partial eclipse of July, 30,1981. Two dimensional power spectrum per unit frequency area (arcsec^2) was fonund to be proportional to exp (-1.9f) where f is the frequency (cycles/arcsec). Further the autocorrelation function as determined from the earlier balloon flight with the use of a 10cm telescope showed a positive maximum around 24∿45Mm, which roughly coincides with the size of the supergranulation. | |||||
ISSN | ||||||
収録物識別子タイプ | ISSN | |||||
収録物識別子 | 0285-9920 | |||||
書誌レコードID | ||||||
収録物識別子タイプ | NCID | |||||
収録物識別子 | AN00354485 | |||||
資料番号 | ||||||
内容記述タイプ | Other | |||||
内容記述 | 資料番号: SA0166572000 |