{"created":"2023-06-20T15:04:00.752584+00:00","id":33217,"links":{},"metadata":{"_buckets":{"deposit":"033d7623-2d27-4a45-86a1-b20d2192244e"},"_deposit":{"created_by":1,"id":"33217","owners":[1],"pid":{"revision_id":0,"type":"depid","value":"33217"},"status":"published"},"_oai":{"id":"oai:jaxa.repo.nii.ac.jp:00033217","sets":["1887:1890","1896:1898:1899:1912"]},"author_link":["415522","415517","415519","415512","415524","415525","415516","415515","415510","415513","415511","415523","415520","415514","415521","415518"],"item_9_alternative_title_2":{"attribute_name":"その他のタイトル（英）","attribute_value_mlt":[{"subitem_alternative_title":"High Energy Primary Electrons Beyond 100GeV"}]},"item_9_biblio_info_10":{"attribute_name":"書誌情報","attribute_value_mlt":[{"bibliographicIssueDates":{"bibliographicIssueDate":"1999-03","bibliographicIssueDateType":"Issued"},"bibliographicPageEnd":"130","bibliographicPageStart":"107","bibliographicVolumeNumber":"39","bibliographic_titles":[{"bibliographic_title":"宇宙科学研究所報告. 特集: 大気球研究報告"}]}]},"item_9_description_16":{"attribute_name":"抄録","attribute_value_mlt":[{"subitem_description":"宇宙線中の高エネルギー電子は銀河中を伝搬中にシンクロトロン過程や, 逆コンプトン効果を受けて, エネルギーを失う。エネルギー損失の度合いはほぼエネルギーの二乗に比例するので, エネルギーの高い電子は源のスペクトルに比べて大きく減少する。このような理由で, 電子線の観測は宇宙線の伝搬に貴重な知見をもたらすものとしてその発見以来数多くの観測がなされてきた。しかし100GeV以上の電子のフラックスが少ないことに加えて, 陽子成分によるシャワーの排除が難しく, 我々のエマルションチャンバーでの観測以外にはこれ迄ほとんど成功していない。しかし, 100GeV以上の電子スペクトルの統計精度はまだ不十分で, このため長時間フライトによる観測を行い, データの集積を行っているところである。1996年9月に三陸から放球したB120-2では平均観測高度37.4kmで34時間52分に及ぶフライトに成功し, その解析を行った。この結果数百GeVの領域で, 観測データの統計的精度は著しく向上させることが出来た。新しく得られた電子スペクトルと, 解析にあたって問題となる陽子の排除率, 高エネルギー領域におけるLPM効果の考察, 電子観測の宇宙物理学的意義などについてやや詳しく述べる。","subitem_description_type":"Abstract"}]},"item_9_description_17":{"attribute_name":"抄録（英）","attribute_value_mlt":[{"subitem_description":"High energy cosmic-ray electrons lose their energy by synchrotron and inverse Compton process during their propagation through the Galaxy. Then the electron spectrum brings us unique information about the sources and propagation of cosmic-rays. Many observations have been carried out since the first discovery of cosmic-ray electrons. Beyond 100GeV, however, only a few observations were successful to observe the absolute flux of electrons. The Emulsion Chamber observations in collaboration with the Washington University group were the most successful to observe the spectrum extending up to a few TeV region. Beyond 100GeV, the statistical accuracy of the observed data is still limited, and we tried to accumulate the data by improving the method of detection of electrons, particularly in a few hundred GeV regions. We report here the results based on new flight exposures of the chamber in 1996. The statistical accuracy of electron spectrum was much improved at several hundred GeV. In this paper, some characteristics of the emulsion chamber compared with counter instruments are summarized. The rejection power for the cosmic-ray protons are analyzed in some detail. The astrophysical significances of the primary electron spectrum are also discussed.","subitem_description_type":"Other"}]},"item_9_description_32":{"attribute_name":"資料番号","attribute_value_mlt":[{"subitem_description":"資料番号: SA0167146000","subitem_description_type":"Other"}]},"item_9_publisher_8":{"attribute_name":"出版者","attribute_value_mlt":[{"subitem_publisher":"宇宙科学研究所"}]},"item_9_publisher_9":{"attribute_name":"出版者（英）","attribute_value_mlt":[{"subitem_publisher":"Institute of Space and Astronautical Science"}]},"item_9_source_id_21":{"attribute_name":"ISSN","attribute_value_mlt":[{"subitem_source_identifier":"0285-9920","subitem_source_identifier_type":"ISSN"}]},"item_9_source_id_24":{"attribute_name":"書誌レコードID","attribute_value_mlt":[{"subitem_source_identifier":"AN00354485","subitem_source_identifier_type":"NCID"}]},"item_9_text_6":{"attribute_name":"著者所属","attribute_value_mlt":[{"subitem_text_value":"青山学院大学理工学部物理"},{"subitem_text_value":"神奈川衛生短大"},{"subitem_text_value":"東京大学宇宙線研究所"},{"subitem_text_value":"神奈川大学"},{"subitem_text_value":"神奈川大学"},{"subitem_text_value":"神奈川大学"},{"subitem_text_value":"神奈川大学"},{"subitem_text_value":"山形工科アカデミー"}]},"item_creator":{"attribute_name":"著者","attribute_type":"creator","attribute_value_mlt":[{"creatorNames":[{"creatorName":"小林, 正"}],"nameIdentifiers":[{}]},{"creatorNames":[{"creatorName":"古森, 良志子"}],"nameIdentifiers":[{}]},{"creatorNames":[{"creatorName":"湯田, 利典"}],"nameIdentifiers":[{}]},{"creatorNames":[{"creatorName":"白井, 達也"}],"nameIdentifiers":[{}]},{"creatorNames":[{"creatorName":"平良, 俊雄"}],"nameIdentifiers":[{}]},{"creatorNames":[{"creatorName":"立山, 暢人"}],"nameIdentifiers":[{}]},{"creatorNames":[{"creatorName":"吉田, 健二"}],"nameIdentifiers":[{}]},{"creatorNames":[{"creatorName":"西村, 純"}],"nameIdentifiers":[{}]},{"creatorNames":[{"creatorName":"KOBAYASHI, Tadashi","creatorNameLang":"en"}],"nameIdentifiers":[{}]},{"creatorNames":[{"creatorName":"KOMORI, Yoshiko","creatorNameLang":"en"}],"nameIdentifiers":[{}]},{"creatorNames":[{"creatorName":"YUDA, Tosinori","creatorNameLang":"en"}],"nameIdentifiers":[{}]},{"creatorNames":[{"creatorName":"SHIRAI, Tatsuya","creatorNameLang":"en"}],"nameIdentifiers":[{}]},{"creatorNames":[{"creatorName":"TAIRA, Toshio","creatorNameLang":"en"}],"nameIdentifiers":[{}]},{"creatorNames":[{"creatorName":"TATEYAMA, Nobuhio","creatorNameLang":"en"}],"nameIdentifiers":[{}]},{"creatorNames":[{"creatorName":"YOSHIDA, Kenji","creatorNameLang":"en"}],"nameIdentifiers":[{}]},{"creatorNames":[{"creatorName":"NISHIMURA, Jun","creatorNameLang":"en"}],"nameIdentifiers":[{}]}]},"item_files":{"attribute_name":"ファイル情報","attribute_type":"file","attribute_value_mlt":[{"accessrole":"open_date","date":[{"dateType":"Available","dateValue":"2020-01-24"}],"displaytype":"detail","filename":"SA0167146.pdf","filesize":[{"value":"1.5 MB"}],"format":"application/pdf","licensetype":"license_note","mimetype":"application/pdf","url":{"label":"SA0167146.pdf","url":"https://jaxa.repo.nii.ac.jp/record/33217/files/SA0167146.pdf"},"version_id":"02a6da2e-42f2-4b31-80b9-d60449d8f7c6"}]},"item_keyword":{"attribute_name":"キーワード","attribute_value_mlt":[{"subitem_subject":"一次電子","subitem_subject_scheme":"Other"},{"subitem_subject":"エマルションチャンバー","subitem_subject_scheme":"Other"},{"subitem_subject":"宇宙線源","subitem_subject_scheme":"Other"},{"subitem_subject":"伝搬モデル","subitem_subject_scheme":"Other"},{"subitem_subject":"LPM効果","subitem_subject_scheme":"Other"}]},"item_language":{"attribute_name":"言語","attribute_value_mlt":[{"subitem_language":"jpn"}]},"item_resource_type":{"attribute_name":"資源タイプ","attribute_value_mlt":[{"resourcetype":"departmental bulletin paper","resourceuri":"http://purl.org/coar/resource_type/c_6501"}]},"item_title":"100GeV 以上の高エネルギーの宇宙線電子について","item_titles":{"attribute_name":"タイトル","attribute_value_mlt":[{"subitem_title":"100GeV 以上の高エネルギーの宇宙線電子について"}]},"item_type_id":"9","owner":"1","path":["1890","1912"],"pubdate":{"attribute_name":"公開日","attribute_value":"2015-03-26"},"publish_date":"2015-03-26","publish_status":"0","recid":"33217","relation_version_is_last":true,"title":["100GeV 以上の高エネルギーの宇宙線電子について"],"weko_creator_id":"1","weko_shared_id":-1},"updated":"2023-06-21T00:12:33.992387+00:00"}