{"created":"2023-06-20T15:28:27.816226+00:00","id":7536,"links":{},"metadata":{"_buckets":{"deposit":"a72250c7-33b6-475c-b82a-494df80f9bb5"},"_deposit":{"created_by":3,"id":"7536","owners":[3],"pid":{"revision_id":0,"type":"depid","value":"7536"},"status":"published"},"_oai":{"id":"oai:ouj.repo.nii.ac.jp:00007536","sets":["470:394:437"]},"author_link":["9598","9599"],"item_10002_biblio_info_7":{"attribute_name":"書誌情報","attribute_value_mlt":[{"bibliographicIssueDates":{"bibliographicIssueDate":"2010-03-23","bibliographicIssueDateType":"Issued"},"bibliographicPageEnd":"126","bibliographicPageStart":"117","bibliographicVolumeNumber":"27","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":"　おうし座RV型星は、主極小と副極小を交互にくり返す光度変化に特徴がある半規則的な変光星である。この変光星は、光度曲線をもとにRVa型とRVb型に細分類されており、RVb型が脈動周期に重なって長周期の光度変化を示すのに対して、RVa型はそのような長周期変化を示さない。またこの変光星は可視域のスペクトルをもとに、酸素過剰なAグループと炭素過剰なB，Cグループに細分類されている。\n　われわれは、岡山天体物理観測所の188cm反射望遠鏡に偏光分光測光装置（HBS）を取り付けて、明るい4個のおうし座RV型星の偏光分光観測を行った。そして、それぞれの星に対して星間偏光を差し引いて固有偏光を求め、固有偏光の波長依存性に関して次の結果を得た。\n（1）HBSで求めたふたご座SS星の固有偏光の波長依存性には3つのタイプがある。それらは脈動変光の位相の違いによると思われる。\n（2）HBSで求めたいっかくじゅう座U星の固有偏光の波長依存性には4つのタイプがある。それらは長周期光度変化の位相の違いによると思われる。\n（3）HBSで求めたオリオン座CT星の固有偏光の波長依存性は、多色偏光測光装置（MCP）で求めた結果に等しい。したがって、オリオン座CT星の固有偏光は時間的に一定と思われる。\n（4）HBSで求めたおうし座座TV星の固有偏光の波長依存性には4つのタイプがある。それらは長周期光度変化の位相の違いによると思われる。ただし、MCPで求めた両者の相関関係とは異なっている。","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":"　The RV Tauri stars are semiregular variables whose light curves are characterized by alternate deep and shallow minima. On the basis of light curve the RV Tauri stars are divided into the RVa group and the RVb group. The RVb group is characterized by a long-term light variation superposed on pulsation period. The RVa group do not show such a long-term variation. On the basis of spectroscopic characteristics in an optical region the RV Tauri stars are divided into the oxygen-rich group, the group A, and the carbon-rich group, the group B and the group C.\n　We newly made the spectropolarimetric observations of 4 bright RV Tauri stars, SS Gem, U Mon, CT Ori, and RV Tau, using 188cm reflector attached with the spectropolarimeter (HBS) at the Okayama Astrophysical Observatory of the National Astronomical Observatory in Japan. We determined intrinsic polarizations for these stars by removing interstellar polarizations and we obtained the following results about the wavelength dependence of intrinsic polarization.\n　1)　There are three types of wavelength dependence of intrinsic polarization of SS Gem observed with HBS. These dependences seem to be due to the difference in phase of the formal period.\n　2)　There are four types of wavelength dependence of intrinsic polarization of U Mon observed with HBS. These wavelength dependences seem to be due to the difference in phase of long-term light variation.\n　3)　The wavelength dependence of CT Ori observed with HBS is the same as that observed with the multi-channel polarimeter (MCP) . Therfore, the intrinsic polarization of CT Ori seems to be constant with time.\n　4)　There are four types of wavelength dependence of intrinsic polarization of RV Tau observed with HBS. These wavelength dependences seem to be due to the difference in phase of long-term light variation, though this correlation between the wavelength dependence and the long-term phase observed with HBS is quite different from that observed with MCP."}]},"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":"9598","nameIdentifierScheme":"WEKO"}]},{"creatorNames":[{"creatorName":"Yoshioka, Kazuo","creatorNameLang":"en"}],"nameIdentifiers":[{"nameIdentifier":"9599","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":"2013-06-14"}],"displaytype":"detail","filename":"27-9.pdf","filesize":[{"value":"1.2 MB"}],"format":"application/pdf","licensetype":"license_note","mimetype":"application/pdf","url":{"label":"27-9","url":"https://ouj.repo.nii.ac.jp/record/7536/files/27-9.pdf"},"version_id":"5bf8f291-0cf2-4d42-8d8e-fd9ccfbf84d5"}]},"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":"HBSでの偏光観測によるおうし座RV型星の長周期変動について","item_titles":{"attribute_name":"タイトル","attribute_value_mlt":[{"subitem_title":"HBSでの偏光観測によるおうし座RV型星の長周期変動について"},{"subitem_title":"Long-Term Periodic Variations in Polarization of RV Tauri Stars Observed with HBS","subitem_title_language":"en"}]},"item_type_id":"10002","owner":"3","path":["437"],"pubdate":{"attribute_name":"公開日","attribute_value":"2013-06-14"},"publish_date":"2013-06-14","publish_status":"0","recid":"7536","relation_version_is_last":true,"title":["HBSでの偏光観測によるおうし座RV型星の長周期変動について"],"weko_creator_id":"3","weko_shared_id":3},"updated":"2023-06-20T16:19:29.153155+00:00"}