{"created":"2021-03-01T06:35:15.250995+00:00","id":27269,"links":{},"metadata":{"_buckets":{"deposit":"84ead437-9c99-4977-a4aa-2ff8698bcf80"},"_deposit":{"id":"27269","owners":[],"pid":{"revision_id":0,"type":"depid","value":"27269"},"status":"published"},"_oai":{"id":"oai:nagoya.repo.nii.ac.jp:00027269","sets":["879:880:881"]},"author_link":["89285","89286","89287","89288","89289","89290"],"item_10_biblio_info_6":{"attribute_name":"書誌情報","attribute_value_mlt":[{"bibliographicIssueDates":{"bibliographicIssueDate":"2019-03","bibliographicIssueDateType":"Issued"},"bibliographicIssueNumber":"3","bibliographicPageStart":"30","bibliographicVolumeNumber":"294","bibliographic_titles":[{"bibliographic_title":"Solar Physics","bibliographic_titleLang":"en"}]}]},"item_10_description_4":{"attribute_name":"抄録","attribute_value_mlt":[{"subitem_description":"We compared the long-term variation (1992–2017) in solar polar brightening observed with the Nobeyama Radioheliograph, the polar solar-wind velocity with interplanetary scintillation observations at the Institute for Space-Earth Environmental Research, and the coronal-hole distribution computed by potential-field calculations of the solar corona using synoptic magnetogram data obtained at the National Solar Observatory/Kitt Peak. First, by comparing the solar-wind velocity [V] and the brightness temperature [Tb] in the polar region, we found good correlation coefficients (CCs) between V and Tb in the polar regions, CC = 0.91 (0.83) for the northern (southern) polar region, and we obtained the V–Tb relationship as V=12.6(Tb−10,667)^1/2+432. We also confirmed that the CC of V–Tb is higher than those of V–B and V–B/f, where B and f are the polar magnetic-field strength and magnetic-flux expansion rate, respectively. These results indicate that Tb is a more direct parameter than B or B/f for expressing solar-wind velocity. Next, we analyzed the long-term variation of the polar brightening and its relation to the area of the polar coronal hole [A]. As a result, we found that the polar brightening matches the probability distribution of the predicted coronal hole and that the CC between Tb and A is remarkably high, CC = 0.97. This result indicates that the polar brightening is strongly coupled to the size of the polar coronal hole. Therefore, the reasonable correlation of V – Tb is explained by V – A. In addition, by considering the anti-correlation between A and f found in a previous study, we suggest that the V – Tb relationship is another expression of the Wang–Sheeley relationship (V – 1/f) in the polar regions.","subitem_description_language":"en","subitem_description_type":"Abstract"}]},"item_10_description_5":{"attribute_name":"内容記述","attribute_value_mlt":[{"subitem_description":"ファイル公開：2020/03/01","subitem_description_language":"ja","subitem_description_type":"Other"}]},"item_10_publisher_32":{"attribute_name":"出版者","attribute_value_mlt":[{"subitem_publisher":"Springer","subitem_publisher_language":"en"}]},"item_10_relation_11":{"attribute_name":"DOI","attribute_value_mlt":[{"subitem_relation_type":"isVersionOf","subitem_relation_type_id":{"subitem_relation_type_id_text":"https://doi.org/10.1007/s11207-019-1418-6","subitem_relation_type_select":"DOI"}}]},"item_10_rights_12":{"attribute_name":"権利","attribute_value_mlt":[{"subitem_rights":"“This is a post-peer-review, pre-copyedit version of an article published in [Solar Physics]. The final authenticated version is available online at: http://dx.doi.org/10.1007/s11207-019-1418-6”.","subitem_rights_language":"en"}]},"item_10_select_15":{"attribute_name":"著者版フラグ","attribute_value_mlt":[{"subitem_select_item":"author"}]},"item_10_source_id_61":{"attribute_name":"ISSN（print）","attribute_value_mlt":[{"subitem_source_identifier":"0038-0938","subitem_source_identifier_type":"PISSN"}]},"item_10_source_id_62":{"attribute_name":"ISSN（Online）","attribute_value_mlt":[{"subitem_source_identifier":"1573-093X","subitem_source_identifier_type":"EISSN"}]},"item_1615787544753":{"attribute_name":"出版タイプ","attribute_value_mlt":[{"subitem_version_resource":"http://purl.org/coar/version/c_ab4af688f83e57aa","subitem_version_type":"AM"}]},"item_access_right":{"attribute_name":"アクセス権","attribute_value_mlt":[{"subitem_access_right":"open access","subitem_access_right_uri":"http://purl.org/coar/access_right/c_abf2"}]},"item_creator":{"attribute_name":"著者","attribute_type":"creator","attribute_value_mlt":[{"creatorNames":[{"creatorName":"Fujiki, Ken’ichi","creatorNameLang":"en"}],"nameIdentifiers":[{"nameIdentifier":"89285","nameIdentifierScheme":"WEKO"}]},{"creatorNames":[{"creatorName":"Shibasaki, Kiyoto","creatorNameLang":"en"}],"nameIdentifiers":[{"nameIdentifier":"89286","nameIdentifierScheme":"WEKO"}]},{"creatorNames":[{"creatorName":"Yashiro, Seiji","creatorNameLang":"en"}],"nameIdentifiers":[{"nameIdentifier":"89287","nameIdentifierScheme":"WEKO"}]},{"creatorNames":[{"creatorName":"Tokumaru, Munetoshi","creatorNameLang":"en"}],"nameIdentifiers":[{"nameIdentifier":"89288","nameIdentifierScheme":"WEKO"}]},{"creatorNames":[{"creatorName":"Iwai, Kazumasa","creatorNameLang":"en"}],"nameIdentifiers":[{"nameIdentifier":"89289","nameIdentifierScheme":"WEKO"}]},{"creatorNames":[{"creatorName":"Masuda, Satoshi","creatorNameLang":"en"}],"nameIdentifiers":[{"nameIdentifier":"89290","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":"2020-03-01"}],"displaytype":"detail","filename":"Fujiki2019SolPhys_accepted.pdf","filesize":[{"value":"1.6 MB"}],"format":"application/pdf","licensetype":"license_note","mimetype":"application/pdf","url":{"label":"Fujiki2019SolPhys_accepted","objectType":"fulltext","url":"https://nagoya.repo.nii.ac.jp/record/27269/files/Fujiki2019SolPhys_accepted.pdf"},"version_id":"d65a406e-47a5-4f62-896f-8564152da9cd"}]},"item_keyword":{"attribute_name":"キーワード","attribute_value_mlt":[{"subitem_subject":"Solar wind","subitem_subject_scheme":"Other"},{"subitem_subject":"Interplanetary scintillation","subitem_subject_scheme":"Other"},{"subitem_subject":"Radioheliograph","subitem_subject_scheme":"Other"},{"subitem_subject":"Coronal holes","subitem_subject_scheme":"Other"},{"subitem_subject":"Magnetic fields","subitem_subject_scheme":"Other"},{"subitem_subject":"Solar Cycle","subitem_subject_scheme":"Other"}]},"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":"journal article","resourceuri":"http://purl.org/coar/resource_type/c_6501"}]},"item_title":"Comparative Study of Microwave Polar Brightening, Coronal Holes, and Solar Wind over the Solar Poles","item_titles":{"attribute_name":"タイトル","attribute_value_mlt":[{"subitem_title":"Comparative Study of Microwave Polar Brightening, Coronal Holes, and Solar Wind over the Solar Poles","subitem_title_language":"en"}]},"item_type_id":"10","owner":"1","path":["881"],"pubdate":{"attribute_name":"PubDate","attribute_value":"2019-03-12"},"publish_date":"2019-03-12","publish_status":"0","recid":"27269","relation_version_is_last":true,"title":["Comparative Study of Microwave Polar Brightening, Coronal Holes, and Solar Wind over the Solar Poles"],"weko_creator_id":"1","weko_shared_id":-1},"updated":"2023-01-16T04:45:27.341754+00:00"}