{"created":"2023-06-20T15:28:21.310025+00:00","id":7386,"links":{},"metadata":{"_buckets":{"deposit":"08b06b0f-d8bd-4e58-9141-6b61e7ae06d9"},"_deposit":{"created_by":3,"id":"7386","owners":[3],"pid":{"revision_id":0,"type":"depid","value":"7386"},"status":"published"},"_oai":{"id":"oai:ouj.repo.nii.ac.jp:00007386","sets":["470:394:447"]},"author_link":["9205","9204"],"item_10002_biblio_info_7":{"attribute_name":"書誌情報","attribute_value_mlt":[{"bibliographicIssueDates":{"bibliographicIssueDate":"1998-03-31","bibliographicIssueDateType":"Issued"},"bibliographicPageEnd":"90","bibliographicPageStart":"71","bibliographicVolumeNumber":"15","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型星は光度曲線をもとに，RVa型とRVb型に分類されている．また，可視域のスペクトルをもとに，酸素過剰のAグループと炭素過剰のB，Cグループに分類され，さらに，AグループはTio帯の有無をもとに，A1，グループとA2グループに細分されている．さらにまた，赤外放射のエネルギー分布をもとに，この星は酸素過剰グループと炭素過剃グループに分類されている．\n　ところが，可視域での分類と赤外放射での分類が必ずしも対応しておらず，可視域で炭素過剰なスペクトルを示しながら，酸素過剰な赤外放射を示すものがある．\n　そこで，両分類の関係を調べるために，おうし座RV型星の多色偏光観測を行っている．観測は，国立天文台堂平観測所の91cm反射望遠鏡に多色偏光測光装置を取り付けて行っている．現在までに17個のおうし座RV型星が観測され，次の結果が得られている。\n1）多くの星で偏光の時間変動が観測され，固有の偏光成分をもつことが確認された．\n2）時間変動の検出率は，RVa型よりもRVb型が高く，また，A2グループよりもA1グループの方が高い．\n3）Aグループでは，偏光度pが中聞の波長域で極大値をもつ傾向があるのに対して，B，Cグループでは，pが中間の波長域で極小値をもつ傾向がある．\n4）U MonやRV　Tauでは，長期的な時間変動が見られる．この変動は周期的で，周期がそれぞれの星の光度変化の振幅の長期的変化の周期に近いようである．\n　以上の結果の解釈も述べられている．","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":"　On tke basis of light curves the RV Tauri stars are divided into the RVa group and the RVb group. On the basis of spectroscopic characteristics in an optical region the RV Tauri stars are divided into the oxygen-rich group, group A, and the carbon-rich group, group B or C. Furthermore, on the basis of the presence of TiO bands the group A are divided into the groups A1 and A2. On the other hand, on the basis of energy distributions of the infrared radiation, RV Tauri stars are divided into the oxygen-rich group and the carbon-rich group.\n　There is not a good correlation between the optical spectra and the infrared spectra for the RV Tauri stars. There are the stars which simultaneously show the carbon-rich optical spectra and the oxygen-rich infrared spectra.\n　The author has been making the multicolor polarimetric observations of the RV Tauri stars in order to clarify the relationship between the optical and the infrared spectra. The 91cm reflector at the Dodaira Station of the National Astronomical Observatory has been used with the multi-channel polarirneter. To date 17 stars have been observed, and the following results are obtained.\n　1) Many stars show the time variations of polarization, which indicates that many stars have intrinsic polarizations.\n　2) Compared with the stars of the RVa group, the stars of the RVb group have a large probability of detection of the time variation of polarization. Furthermore, compared with the stars of the group A2, the stars of the group A1 have a large probability of detection of the time variation of polarization.\n　3) The stars of the A group show a tendency for the p values to take a maximim at an intermediate wavelength, while the stars of the group B or C show a tendency to take a minimum at an intermediate wavelength.\n　4) U Mon and RV Tau show long term time variations of polarization. These variations seems to be periodic, whose periods are close to the periods of the long wave of amplitude of brightness variation.\n　　The interpretations of the results also are given."}]},"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":"9204","nameIdentifierScheme":"WEKO"}]},{"creatorNames":[{"creatorName":"Yoshioka, Kazuo","creatorNameLang":"en"}],"nameIdentifiers":[{"nameIdentifier":"9205","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_15-71-90.pdf","filesize":[{"value":"1.3 MB"}],"format":"application/pdf","licensetype":"license_note","mimetype":"application/pdf","url":{"label":"NO_15-71-90","url":"https://ouj.repo.nii.ac.jp/record/7386/files/NO_15-71-90.pdf"},"version_id":"180fc4d9-73c5-4c35-ae4b-825d65c61174"}]},"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型変光星の偏光の変動について III : われわれの観測の主な結果","item_titles":{"attribute_name":"タイトル","attribute_value_mlt":[{"subitem_title":"おうし座RV型変光星の偏光の変動について III : われわれの観測の主な結果"},{"subitem_title":"Polarization Variations of the RV Tauri Stars III : The Principal Results of Our Observations","subitem_title_language":"en"}]},"item_type_id":"10002","owner":"3","path":["447"],"pubdate":{"attribute_name":"公開日","attribute_value":"2013-06-14"},"publish_date":"2013-06-14","publish_status":"0","recid":"7386","relation_version_is_last":true,"title":["おうし座RV型変光星の偏光の変動について III : われわれの観測の主な結果"],"weko_creator_id":"3","weko_shared_id":3},"updated":"2023-06-20T16:16:33.380254+00:00"}