{"created":"2023-06-20T15:28:37.347767+00:00","id":8055,"links":{},"metadata":{"_buckets":{"deposit":"dfc4cdac-ce03-4c3b-9f5c-654efc217edd"},"_deposit":{"created_by":3,"id":"8055","owners":[3],"pid":{"revision_id":0,"type":"depid","value":"8055"},"status":"published"},"_oai":{"id":"oai:ouj.repo.nii.ac.jp:00008055","sets":["470:394:515"]},"author_link":["10036","10037","10038","10035"],"item_10002_biblio_info_7":{"attribute_name":"書誌情報","attribute_value_mlt":[{"bibliographicIssueDates":{"bibliographicIssueDate":"2014-03-20","bibliographicIssueDateType":"Issued"},"bibliographicPageEnd":"96","bibliographicPageStart":"89","bibliographicVolumeNumber":"31","bibliographic_titles":[{"bibliographic_title":"放送大学研究年報"},{"bibliographic_title":"Journal of the Open University of Japan","bibliographic_titleLang":"en"}]}]},"item_10002_description_5":{"attribute_name":"抄録","attribute_value_mlt":[{"subitem_description":"　惑星を持つ恒星は、惑星を持たない恒星に比べて光球中での重元素の量が多い傾向を持つことが知られている。この傾向の解釈の１つに汚染説がある。\n　われわれは、汚染説の成否を決定する目的で惑星を持つ２つの星、ε EriとHD37124を観測し、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った。整約はソフトアウェアIRAFを用いて行い、解析は吉岡が作成したプログラムを用いて、相対成長曲線法で行った。\n　そして、次の結果が得られた。\n１） 両星とも、太陽に対する相対的な元素量と凝縮温度の関係として、データの散らばりは大きいが、［M/Fe］の値が凝縮温度とともに減少する関係が成り立つ。\n２） スペクトル型がK2V型のε Eriの方が、スペクトル型がG4V型のHD37124よりも上述の傾向が顕著である。\n　これらの結果は、汚染説から導かれる予測に反している。しかし、原始惑星系星雲の時期に揮発性元素と不揮発性元素の分離が起こり、揮発性元素の光球への降着が起きなかったとする、別の観点からの予測には反していない。","subitem_description_type":"Abstract"}]},"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":"　It is known that host stars with planets have a tendency to have a large metallic abundance in their photospheres in comparison with stars without planets. One of the explanations for this tendency is the self-enrichment explanation.\n　We observed two stars with planets, ε Eri and HD37124, and we determined the chemical abundances of these stars in order to decide the right or wrong of the self-enrichment explanation.\n　The observations were made with the Echelle Spectrograph attached to the 150cm reflector at Gunma Astronomical Observatory in Gunma prefecture in Japan. Data reduction was carried out using standard techniques within the IRAF image processing software. The analysis was done by a sort of the differential curve-of-growth method, 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 stars that the［ M/Fe］ values decrease with the condensation temperature, thought the scatters are large.\n2） The above correlation of the K2V star, ε Eri, is more conspicuous than that of the G4V star, HD37124.\n　These results are contrary to the expectations from the self-enrichment explanation. However, these results are not contrary to the expectations from other viewpoint that the fractionation of volatile and refractory elements may have occurred in the protoplanetary nebulae and significant accretion of refractory rich planet material has not taken place.\n　It is desired that more stars with planets are observed and more precise observations are done in order to decide the right or wrong of the self-enrichment explanation."}]},"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":"10035","nameIdentifierScheme":"WEKO"}]},{"creatorNames":[{"creatorName":"山口, 直晃"},{"creatorName":"ヤマグチ, ナオアキ","creatorNameLang":"ja-Kana"}],"nameIdentifiers":[{"nameIdentifier":"10036","nameIdentifierScheme":"WEKO"}]},{"creatorNames":[{"creatorName":"Yoshioka, Kazuo","creatorNameLang":"en"}],"nameIdentifiers":[{"nameIdentifier":"10037","nameIdentifierScheme":"WEKO"}]},{"creatorNames":[{"creatorName":"Yamaguchi, Naoaki","creatorNameLang":"en"}],"nameIdentifiers":[{"nameIdentifier":"10038","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":"2014-04-25"}],"displaytype":"detail","filename":"31_09.pdf","filesize":[{"value":"262.3 kB"}],"format":"application/pdf","licensetype":"license_note","mimetype":"application/pdf","url":{"label":"31_09","url":"https://ouj.repo.nii.ac.jp/record/8055/files/31_09.pdf"},"version_id":"278d96d1-8676-401f-83f8-04fe2d5306dc"}]},"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":"惑星を持つ２つの恒星、エリダヌス座ε星とHD37124の化学組成の決定","item_titles":{"attribute_name":"タイトル","attribute_value_mlt":[{"subitem_title":"惑星を持つ２つの恒星、エリダヌス座ε星とHD37124の化学組成の決定"},{"subitem_title":"The Determination of Abundances of Two Stars with Planets, ε Eri and HD37124","subitem_title_language":"en"}]},"item_type_id":"10002","owner":"3","path":["515"],"pubdate":{"attribute_name":"公開日","attribute_value":"2014-04-25"},"publish_date":"2014-04-25","publish_status":"0","recid":"8055","relation_version_is_last":true,"title":["惑星を持つ２つの恒星、エリダヌス座ε星とHD37124の化学組成の決定"],"weko_creator_id":"3","weko_shared_id":3},"updated":"2023-06-20T16:14:41.322246+00:00"}