{"created":"2023-06-20T15:28:26.716118+00:00","id":7510,"links":{},"metadata":{"_buckets":{"deposit":"bc663643-0b08-495c-91d0-28a12e50aa97"},"_deposit":{"created_by":3,"id":"7510","owners":[3],"pid":{"revision_id":0,"type":"depid","value":"7510"},"status":"published"},"_oai":{"id":"oai:ouj.repo.nii.ac.jp:00007510","sets":["470:394:435"]},"author_link":["9538","9539"],"item_10002_biblio_info_7":{"attribute_name":"書誌情報","attribute_value_mlt":[{"bibliographicIssueDates":{"bibliographicIssueDate":"2008-03-20","bibliographicIssueDateType":"Issued"},"bibliographicPageEnd":"136","bibliographicPageStart":"127","bibliographicVolumeNumber":"25","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グループとCグループに細分類されている。\n　われわれは、国立天文台の堂平観測所と岡山天体物理観測所の91cm反射望遠鏡に偏光分光測光装置（HBS）を取り付けて、明るい5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、次の結果を得た。\n　ふたご座SS星といっかくじゅう座U星とおうし座RV星では、固有偏光度の波長依存性に時間変動が見られる。\n　上記の時間変動の多くには脈動の位相との相関が見られないが、長周期光度変化と相関がありそうな星がある。\n　いっかくじゅう座U星のいくつかの観測では、その固有偏光度にいくつかの波長でピークが見られ、ピークの波長が放射の吸収帯に一致している。\n　ふたご座SS星とヘルクレス座AC星とおうし座RV星では、固有偏光位置角にも波長依存性が見られる。とくにおうし座RV星では、長周期光度変化の増光期に5500Å付近よりも短波長側で固有偏光位置角が波長とともに減少している。この波長依存性は、たて座R星の過去の偏光分光観測で観測されたものに似ている。","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 made the spectropolarimetric observations of 5 bright RV Tauri stars, using 91cm reflectors attached with the spectropolarimeter (HBS) at the Dodaira Station and the Okayama Astrophysical Observatory of the Natioltal Astronomical Observatory in Japan. We determined intrinsic polarizations for these stars by removing interstellar polarizations and we obtained the following results.\n　1) SS Gem, U Mon, and RV Tau show the time variation in wavelength dependence of the degree of intrinsic polarization.\n　2) Many of the above variations do not correlate with the phase of pulsation, and for some stars the above variation may correlate with the phase of long-term light variation.\n　3) Some observations of U Mon show that the degree of intrinsic polarization have several peaks and the wavelength of the peaks coincide with those of the dips in flux distribution.\n　4) For SS Gem, AC Her, and RV Tau, the position angle of intrinsic polarization show a wavelength dependence. Especially for RV Tau, the angle for the wavelength shorter than about 5500Å decreases with wavelength at the brightening phase of long-term light variation, which dependence resembles that for R Sct obtained before by spectropolarimetrical observation."}]},"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":"9538","nameIdentifierScheme":"WEKO"}]},{"creatorNames":[{"creatorName":"Yoshioka, Kazuo","creatorNameLang":"en"}],"nameIdentifiers":[{"nameIdentifier":"9539","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":"25-014.pdf","filesize":[{"value":"1.2 MB"}],"format":"application/pdf","licensetype":"license_note","mimetype":"application/pdf","url":{"label":"25-014","url":"https://ouj.repo.nii.ac.jp/record/7510/files/25-014.pdf"},"version_id":"3559210e-6096-4562-92b6-6b18cef3baf2"}]},"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":"おうし座RV型星のHBS(偏光分光測光装置)による偏光観測とその固有偏光","item_titles":{"attribute_name":"タイトル","attribute_value_mlt":[{"subitem_title":"おうし座RV型星のHBS(偏光分光測光装置)による偏光観測とその固有偏光"},{"subitem_title":"Polarimetric Observations of the RV Tauri Stars with HBS (Hennko Bunnko Sokkosochi)and Their Intrinsic Polarizations","subitem_title_language":"en"}]},"item_type_id":"10002","owner":"3","path":["435"],"pubdate":{"attribute_name":"公開日","attribute_value":"2013-06-14"},"publish_date":"2013-06-14","publish_status":"0","recid":"7510","relation_version_is_last":true,"title":["おうし座RV型星のHBS(偏光分光測光装置)による偏光観測とその固有偏光"],"weko_creator_id":"3","weko_shared_id":3},"updated":"2023-06-20T16:18:38.090814+00:00"}