{"created":"2023-06-20T15:03:53.086471+00:00","id":33081,"links":{},"metadata":{"_buckets":{"deposit":"8bd602a4-52ef-48e7-8bce-4eeac4cb8c12"},"_deposit":{"created_by":1,"id":"33081","owners":[1],"pid":{"revision_id":0,"type":"depid","value":"33081"},"status":"published"},"_oai":{"id":"oai:jaxa.repo.nii.ac.jp:00033081","sets":["1887:1890","1896:1898:1899:1912"]},"author_link":["414070","414069","414071","414073","414072"],"item_9_alternative_title_2":{"attribute_name":"その他のタイトル（英）","attribute_value_mlt":[{"subitem_alternative_title":"X-ray spectral feature from Seyfert galaxies"}]},"item_9_biblio_info_10":{"attribute_name":"書誌情報","attribute_value_mlt":[{"bibliographicIssueDates":{"bibliographicIssueDate":"1990-01","bibliographicIssueDateType":"Issued"},"bibliographicPageEnd":"239","bibliographicPageStart":"229","bibliographicVolumeNumber":"25","bibliographic_titles":[{"bibliographic_title":"宇宙科学研究所報告. 特集: 宇宙観測研究報告"}]}]},"item_9_description_16":{"attribute_name":"抄録","attribute_value_mlt":[{"subitem_description":"これまでに「ぎんが」衛星によって観測されたいくつかのI型セイファート銀河からのX線放射のスペクトルには, 7-10keV付近に吸収端のような形と, 約10keV以上が盛り上がる構造の存在することが新たに見つかった。このようなX線スペクトルはこれまでに唱えられてきたような標準的なモデル, 即ちべき関数的にエネルギー分布する放射が一様なガスによって吸収を受けているというモデルでは説明することが出来ない。このようなスペクトルの構造は, 吸収ガスが一様ではなくX線源の一部だけを覆うような濃いガスが存在しているために, 強い吸収を受けた成分と強い吸収を受けていない成分とが重なってできたもの(部分吸収モデル), もしくは, より高エネルギー部の放射が濃いガスによって何回かコンプトン散乱され, 反射されて直接成分に重なってできたもの(コンプトン反射モデル)と考えるのがもっともらしいことがわかった。いずれにしてもコラム密度10^<24>cm^<-2>以上の濃いガスがX線源の周りに存在していることを示唆し, これまでの活動銀河核で唱えられてきたBLR (Bload Line Region)とNLR (Nallow Line Region)のモデルに何らかの濃いガスの領域を導入しなければならないことになる。","subitem_description_type":"Abstract"}]},"item_9_description_17":{"attribute_name":"抄録（英）","attribute_value_mlt":[{"subitem_description":"In the X-ray spectra from some Seyfert-I galaxies observed with the GINGA satellite, the existence of an absorption-like feature at 7-10keV and hard X-ray component above 10keV have been discoverd. These X-ray spectra cannot be explained by the standard model where the rediation emitted with a power-law form is absorded by uniform matter. These features in the spectra are most likely explained by a partial covering model or by a Compton reflection model. In the partial covering model the absorber is not uniformly distributed but consists of blobs which partially cover the X-ray source. The feature in the spectrum may be formed by the combination of direct and highly adsorbed X-rays. On the other hand, in the Compton reflection model the feature may be formed by the composition of direct X-rays and refiected X-rays which come from more energetic radiation via repeated Compton scatterings. These models suggest the existence of thick gas of more than 10^<24>cm^<-2> around the X-ray source.","subitem_description_type":"Other"}]},"item_9_description_32":{"attribute_name":"資料番号","attribute_value_mlt":[{"subitem_description":"資料番号: SA0166940000","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":"理化学研究所"},{"subitem_text_value":"理化学研究所"},{"subitem_text_value":"理化学研究所"}]},"item_creator":{"attribute_name":"著者","attribute_type":"creator","attribute_value_mlt":[{"creatorNames":[{"creatorName":"山内, 誠"}],"nameIdentifiers":[{}]},{"creatorNames":[{"creatorName":"松岡, 勝"}],"nameIdentifiers":[{}]},{"creatorNames":[{"creatorName":"YAMAUCHI, M.","creatorNameLang":"en"}],"nameIdentifiers":[{}]},{"creatorNames":[{"creatorName":"MATSUOKA, M.","creatorNameLang":"en"}],"nameIdentifiers":[{}]},{"creatorNames":[{"creatorName":"PIRO, L.","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":"SA0166940.pdf","filesize":[{"value":"631.2 kB"}],"format":"application/pdf","licensetype":"license_note","mimetype":"application/pdf","url":{"label":"SA0166940.pdf","url":"https://jaxa.repo.nii.ac.jp/record/33081/files/SA0166940.pdf"},"version_id":"66661914-2729-446d-a5aa-0516f6fafc58"}]},"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":"セイファート銀河の X 線スペクトルの構造","item_titles":{"attribute_name":"タイトル","attribute_value_mlt":[{"subitem_title":"セイファート銀河の X 線スペクトルの構造"}]},"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":"33081","relation_version_is_last":true,"title":["セイファート銀河の X 線スペクトルの構造"],"weko_creator_id":"1","weko_shared_id":-1},"updated":"2023-06-21T00:16:10.507873+00:00"}