{"created":"2023-06-20T15:28:49.318072+00:00","id":8359,"links":{},"metadata":{"_buckets":{"deposit":"2cbbf392-e613-42ca-aace-5e58cab655be"},"_deposit":{"created_by":12,"id":"8359","owners":[12],"pid":{"revision_id":0,"type":"depid","value":"8359"},"status":"published"},"_oai":{"id":"oai:ouj.repo.nii.ac.jp:00008359","sets":["470:394:542"]},"author_link":["10613","10611","10614","10612"],"item_10002_biblio_info_7":{"attribute_name":"書誌情報","attribute_value_mlt":[{"bibliographicIssueDates":{"bibliographicIssueDate":"2015-03-20","bibliographicIssueDateType":"Issued"},"bibliographicPageEnd":"125","bibliographicPageStart":"117","bibliographicVolumeNumber":"32","bibliographic_titles":[{"bibliographic_title":"放送大学研究年報 = Journal of The Open University of Japan"}]}]},"item_10002_description_12":{"attribute_name":"論文ID（NAID）","attribute_value_mlt":[{"subitem_description":"40020473231","subitem_description_type":"Other"}]},"item_10002_description_5":{"attribute_name":"抄録","attribute_value_mlt":[{"subitem_description":"　われわれは、おうし座RV型変光星の化学組成の異常を説明する３つの説の当否を決めるため、２個のおうし座RV\n型変光星、AC HerとRV Tauを観測し、これらの星の化学組成を求めた。\n　観測は、県立ぐんま天文台の150cm反射望遠鏡に取り付けたエッシェル分光器を用いて行い、解析は吉岡が作成し\nたプログラムを用いて、太陽を比較星とする一種の相対成長曲線法で行った。整約はソフトアウェアIRAFを用いて\n行った。\n　そして、次の結果が得られた。\n１） 両星とも太陽に相対的な元素量は、散らばりは大きいが、凝縮温度と相関関係を示し、［M/H］の値は凝縮温度\nが高いほど少ない。この結果は、両星ともダスト・ガス凝縮が働いていることを示してる。\n２） 上述の相関は、AグループのRV Tauの方がBグループのAC Herよりも顕著である。これは、Bグループの星に\nはダスト・ガス凝縮が見られるが、Aグループの星には明確には見られない、というGiridhar et al.（ 2000）18）の\n結果に反する。\n３） AC HerとRV Tauの［S/H］と［Zn/H］の値によれば、２）の結果は、もともとの［Fe/H］の値が－1よりも小さな\npost-AGB星はダスト・ガス凝縮の影響を受けない、というGiridhar et al（. 2000）18）の結果には反しない。\n４） 両星とも相対的な元素量が各元素の第１電離ポテンシャルと相関関係が見られず、第１電離機構が働いていない\nことを示している。\n５） 両星とも相対的な元素量が各元素の第２電離ポテンシャルと相関関係が見られず、第２電離機構が働いていない\nことを示している。\n　以上の結果を確認するために、成長曲線法の異なる方式で再解析することが望まれる。","subitem_description_type":"Abstract"}]},"item_10002_publisher_8":{"attribute_name":"出版者","attribute_value_mlt":[{"subitem_publisher":"放送大学"}]},"item_10002_source_id_11":{"attribute_name":"書誌レコードID","attribute_value_mlt":[{"subitem_source_identifier":"AN10019636","subitem_source_identifier_type":"NCID"}]},"item_10002_source_id_9":{"attribute_name":"ISSN","attribute_value_mlt":[{"subitem_source_identifier":"0911-4505","subitem_source_identifier_type":"ISSN"}]},"item_10002_textarea_25":{"attribute_name":"抄録（英）","attribute_value_mlt":[{"subitem_textarea_language":"en","subitem_textarea_value":"　We observed two RV Tauri variables, AC Her and RV Tau, and we determined the chemical abundance of these\nstars in order to decide the right or wrong of the three proposed mechanisms which explain the anomalous chemical\nabundance of the RV Tauri variables.\n　The observations were made with the Echelle Spectrograph attached to the 150cm reflector at Gunma\nAstronomical Observatory in Gunma prefecture in Japan. Data reduction was carried out using standard techniques\nwith the IRAF image processing software. The analysis was done by a sort of the differential curve-of-growth\nmethod, where the sun was selected as the comparison star, using the program made by Yoshioka.\n　The following results were obtained.\n1） There is a correlation between the abundance relative to the sun and the condensation temperature for both of the\nstars that the［ M/H］ values decrease with the condensation temperature, thought the scatters are large, which\nindicates that the dust-gas separation mechanism prevails in both of the stars.\n2） The above correlation of the group A star, RV Tau, is more conspicuous than that of the group B star, AC Her,\nwhich contradicts the results by Giridhar et al.（ 2000）18）, who observed that the group B show the pattern of\nabundance ascribed to the dust-gas separation mechanism, but the stars of the group A show the abundance\nwhich are very largely unaffected by the dust-gas separation mechanism.\n3）A ccording to our mean values of［ S/H］ and［ Zn/H］ for AC Her and RV Tau, the above result of 2） do not\ncontradict the results by Giridhar et al.（ 2000）18）, who observed that the post-AGB stars with an intrinsic［ Fe/H］\nlower than －1 are not subject to the effects of the dust-gas separation.\n4） There is not a correlation between the relative abundance and the first ionization potential of the element for both\nof the stars, which indicates that the first ionization mechanism does not prevails in both of the stars.\n5） There is not a correlation between the relative abundance and the second ionization potential of the element for\nboth of the stars, which indicates that the second ionization mechanism does not prevails in both of the stars.\n　It is desired that these stars should be reanalyzed by a different process of the differential curve-of-growth\nanalysis, in order to confirm our results."}]},"item_10002_version_type_20":{"attribute_name":"著者版フラグ","attribute_value_mlt":[{"subitem_version_resource":"http://purl.org/coar/version/c_970fb48d4fbd8a85","subitem_version_type":"VoR"}]},"item_creator":{"attribute_name":"著者","attribute_type":"creator","attribute_value_mlt":[{"creatorNames":[{"creatorName":"吉岡, 一男"},{"creatorName":"ヨシオカ, カズオ","creatorNameLang":"ja-Kana"}],"nameIdentifiers":[{"nameIdentifier":"10611","nameIdentifierScheme":"WEKO"},{"nameIdentifier":"1000060158392","nameIdentifierScheme":"NRID","nameIdentifierURI":" "}]},{"creatorNames":[{"creatorName":"松田, 利通"},{"creatorName":"マツダ, トシミチ","creatorNameLang":"ja-Kana"}],"nameIdentifiers":[{"nameIdentifier":"10612","nameIdentifierScheme":"WEKO"}]},{"creatorNames":[{"creatorName":"Yoshioka, Kazuo","creatorNameLang":"en"}],"nameIdentifiers":[{"nameIdentifier":"10613","nameIdentifierScheme":"WEKO"}]},{"creatorNames":[{"creatorName":"Matsuda, Toshimiti","creatorNameLang":"en"}],"nameIdentifiers":[{"nameIdentifier":"10614","nameIdentifierScheme":"WEKO"}]}]},"item_files":{"attribute_name":"ファイル情報","attribute_type":"file","attribute_value_mlt":[{"accessrole":"open_date","date":[{"dateType":"Available","dateValue":"2015-10-20"}],"displaytype":"detail","filename":"32_10.pdf","filesize":[{"value":"251.1 kB"}],"format":"application/pdf","licensetype":"license_note","mimetype":"application/pdf","url":{"label":"２つのおうし座RV型変光星、ヘルクレス座AC星とおうし座TV星の化学組成の決定","url":"https://ouj.repo.nii.ac.jp/record/8359/files/32_10.pdf"},"version_id":"763dfe91-643d-46e2-b161-e38575c037c6"}]},"item_language":{"attribute_name":"言語","attribute_value_mlt":[{"subitem_language":"eng"}]},"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":"2つのおうし座RV型変光星、 ヘルクレス座AC星とおうし座TV星の化学組成の決定","item_titles":{"attribute_name":"タイトル","attribute_value_mlt":[{"subitem_title":"2つのおうし座RV型変光星、 ヘルクレス座AC星とおうし座TV星の化学組成の決定"},{"subitem_title":"The Determination of Abundances of Two Stars RV Tauri Stars, AC Her and RV Tau","subitem_title_language":"en"}]},"item_type_id":"10002","owner":"12","path":["542"],"pubdate":{"attribute_name":"公開日","attribute_value":"2015-10-20"},"publish_date":"2015-10-20","publish_status":"0","recid":"8359","relation_version_is_last":true,"title":["2つのおうし座RV型変光星、 ヘルクレス座AC星とおうし座TV星の化学組成の決定"],"weko_creator_id":"12","weko_shared_id":-1},"updated":"2023-12-19T06:58:26.376839+00:00"}