{"_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": ["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", "download_preview_message": "", "file_order": 0, "filename": "Fujiki2019SolPhys_accepted.pdf", "filesize": [{"value": "1.6 MB"}], "format": "application/pdf", "future_date_message": "", "is_thumbnail": false, "licensetype": "license_note", "mimetype": "application/pdf", "size": 1600000.0, "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"], "permalink_uri": "http://hdl.handle.net/2237/00029468", "pubdate": {"attribute_name": "PubDate", "attribute_value": "2019-03-12"}, "publish_date": "2019-03-12", "publish_status": "0", "recid": "27269", "relation": {}, "relation_version_is_last": true, "title": ["Comparative Study of Microwave Polar Brightening, Coronal Holes, and Solar Wind over the Solar Poles"], "weko_shared_id": -1}