{"_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"}, "item_10_biblio_info_6": {"attribute_name": "\u66f8\u8a8c\u60c5\u5831", "attribute_value_mlt": [{"bibliographicIssueDates": {"bibliographicIssueDate": "2019-03", "bibliographicIssueDateType": "Issued"}, "bibliographicIssueNumber": "3", "bibliographicPageStart": "30", "bibliographicVolumeNumber": "294", "bibliographic_titles": [{"bibliographic_title": "Solar Physics"}]}]}, "item_10_description_4": {"attribute_name": "\u6284\u9332", "attribute_value_mlt": [{"subitem_description": "We compared the long-term variation (1992\u20132017) 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\u2013Tb relationship as V=12.6(Tb\u221210,667)^1/2+432. We also confirmed that the CC of V\u2013Tb is higher than those of V\u2013B and V\u2013B/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\u2009\u2013\u2009Tb is explained by V\u2009\u2013\u2009A. In addition, by considering the anti-correlation between A and f found in a previous study, we suggest that the V\u2009\u2013\u2009Tb relationship is another expression of the Wang\u2013Sheeley relationship (V\u2009\u2013\u20091/f) in the polar regions.", "subitem_description_type": "Abstract"}]}, "item_10_description_5": {"attribute_name": "\u5185\u5bb9\u8a18\u8ff0", "attribute_value_mlt": [{"subitem_description": "\u30d5\u30a1\u30a4\u30eb\u516c\u958b\uff1a2020/03/01", "subitem_description_type": "Other"}]}, "item_10_publisher_32": {"attribute_name": "\u51fa\u7248\u8005", "attribute_value_mlt": [{"subitem_publisher": "Springer"}]}, "item_10_relation_11": {"attribute_name": "DOI", "attribute_value_mlt": [{"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": "\u6a29\u5229", "attribute_value_mlt": [{"subitem_rights": "\u201cThis 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\u201d."}]}, "item_10_select_15": {"attribute_name": "\u8457\u8005\u7248\u30d5\u30e9\u30b0", "attribute_value_mlt": [{"subitem_select_item": "author"}]}, "item_10_source_id_61": {"attribute_name": "ISSN\uff08print\uff09", "attribute_value_mlt": [{"subitem_source_identifier": "0038-0938", "subitem_source_identifier_type": "ISSN"}]}, "item_10_source_id_62": {"attribute_name": "ISSN\uff08Online\uff09", "attribute_value_mlt": [{"subitem_source_identifier": "1573-093X", "subitem_source_identifier_type": "ISSN"}]}, "item_creator": {"attribute_name": "\u8457\u8005", "attribute_type": "creator", "attribute_value_mlt": [{"creatorNames": [{"creatorName": "Fujiki, Ken\u2019ichi"}], "nameIdentifiers": [{"nameIdentifier": "89285", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Shibasaki, Kiyoto"}], "nameIdentifiers": [{"nameIdentifier": "89286", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Yashiro, Seiji"}], "nameIdentifiers": [{"nameIdentifier": "89287", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Tokumaru, Munetoshi"}], "nameIdentifiers": [{"nameIdentifier": "89288", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Iwai, Kazumasa"}], "nameIdentifiers": [{"nameIdentifier": "89289", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Masuda, Satoshi"}], "nameIdentifiers": [{"nameIdentifier": "89290", "nameIdentifierScheme": "WEKO"}]}]}, "item_files": {"attribute_name": "\u30d5\u30a1\u30a4\u30eb\u60c5\u5831", "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_free", "mimetype": "application/pdf", "size": 1600000.0, "url": {"label": "Fujiki2019SolPhys_accepted", "url": "https://nagoya.repo.nii.ac.jp/record/27269/files/Fujiki2019SolPhys_accepted.pdf"}, "version_id": "d65a406e-47a5-4f62-896f-8564152da9cd"}]}, "item_keyword": {"attribute_name": "\u30ad\u30fc\u30ef\u30fc\u30c9", "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": "\u8a00\u8a9e", "attribute_value_mlt": [{"subitem_language": "eng"}]}, "item_resource_type": {"attribute_name": "\u8cc7\u6e90\u30bf\u30a4\u30d7", "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": "\u30bf\u30a4\u30c8\u30eb", "attribute_value_mlt": [{"subitem_title": "Comparative Study of Microwave Polar Brightening, Coronal Holes, and Solar Wind over the Solar Poles"}]}, "item_type_id": "10", "owner": "1", "path": ["879/880/881"], "permalink_uri": "http://hdl.handle.net/2237/00029468", "pubdate": {"attribute_name": "\u516c\u958b\u65e5", "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": null}