{"created":"2023-06-20T15:28:23.000116+00:00","id":7425,"links":{},"metadata":{"_buckets":{"deposit":"58f5fef3-2282-423c-b607-a257887a7bb3"},"_deposit":{"created_by":3,"id":"7425","owners":[3],"pid":{"revision_id":0,"type":"depid","value":"7425"},"status":"published"},"_oai":{"id":"oai:ouj.repo.nii.ac.jp:00007425","sets":["470:394:444"]},"author_link":["9294","9295"],"item_10002_biblio_info_7":{"attribute_name":"書誌情報","attribute_value_mlt":[{"bibliographicIssueDates":{"bibliographicIssueDate":"2001-03-31","bibliographicIssueDateType":"Issued"},"bibliographicPageEnd":"149","bibliographicPageStart":"133","bibliographicVolumeNumber":"18","bibliographic_titles":[{"bibliographic_title":"放送大学研究年報"},{"bibliographic_title":"Journal of the University of the Air","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脈動変光星である．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型が脈動周期の光度変化に重なって長周期の光度変化が見られるのに対して，RVa型にはそのような長周期変化は見られない．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，国立天文台堂平観測所の91cm反射望遠鏡を用いて，おうし座RV型星の多色偏光観測を行った．観測された17個の星の内，4個の星に対して星間偏光成分を取り除いて固有偏光成分を求めた．星間偏光成分は，near-neighbor法で決定された．われわれが得た星間偏光成分の偏光位置角は，他の観測者の得た値に近いが，われわれが得た星間偏光成分の偏光度のいくつかは，他の観測者の値と大きく異なる．われわれの得た値は，星間偏光に対してより根拠のある仮定に基づいているので，より信頼度が高い．\n　われわれの求めた固有偏光成分は，いっかくじゅう座U星を除き，星周圏ダストの幾何的配置が時間変動をしないことを示唆している．さらにわれわれの結果は，Aグループの星で観測された偏光度が中間の波長で極大値をとる傾向がある，というわれわれがすでに得ている結果を支持している．","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 altenate deep and shallow minima. On the basis of light curves the RV Tauri stars are divided into the RVa and the RVb groups. The RVa group is characterized by a relatively regular light curve, while the RVb group is characterized by a superimposition of a long-term variation. On the basis of spectroscopic characteristics in an optical region the RV Tauri stars are divided lnto the oxygen-rich group, the group A, and the carbon-rich group, the group B and the group C.\n　We made the raulticolor polarimetric observations of RV Tauri stars, using the 91cm reflector at the Dodaira Station of the National Astronomical Observatory. Among 17 stars observed we obtained the intrinsic polarizations of 4 stars by removing the interstellar polarizations. The interstellar polaizations were determined by the near-neighbor method. Our values for the position angle of interstellar polarization are close to those determined by other observers, while some of our values for the degree of interstellar polarization are noticeably differ from those determined by other observers. Our values seem to be more reliable, because our assumptions concerning the interstellar polarization are more founded.\n　The intrinsic polarizations determined by gs suggest that except for U Mon the geometrical arrangement of circumstellar dust envelope do not change with time. Furthermore, our results confirm the tendency for the degree of observed polarization for the stars belonging to the group A to take a maximum at an intermediate wavelength, which were observed by us."}]},"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":"9294","nameIdentifierScheme":"WEKO"}]},{"creatorNames":[{"creatorName":"Yoshioka, Kazuo","creatorNameLang":"en"}],"nameIdentifiers":[{"nameIdentifier":"9295","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":"NO_18-133-149.pdf","filesize":[{"value":"1.1 MB"}],"format":"application/pdf","licensetype":"license_note","mimetype":"application/pdf","url":{"label":"NO_18-133-149","url":"https://ouj.repo.nii.ac.jp/record/7425/files/NO_18-133-149.pdf"},"version_id":"63a2c232-e3d8-4b23-9ae5-1291535c6d5c"}]},"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":"4個のおうし座RV型星の固有偏光の特徴について","item_titles":{"attribute_name":"タイトル","attribute_value_mlt":[{"subitem_title":"4個のおうし座RV型星の固有偏光の特徴について"},{"subitem_title":"The characteristics of intrinsic polarization for four RV Tauri stars","subitem_title_language":"en"}]},"item_type_id":"10002","owner":"3","path":["444"],"pubdate":{"attribute_name":"公開日","attribute_value":"2013-06-14"},"publish_date":"2013-06-14","publish_status":"0","recid":"7425","relation_version_is_last":true,"title":["4個のおうし座RV型星の固有偏光の特徴について"],"weko_creator_id":"3","weko_shared_id":3},"updated":"2023-06-20T16:17:03.630796+00:00"}