{"_buckets": {"deposit": "9fe1659c-1162-4906-a72e-79f1ead24a82"}, "_deposit": {"id": "25997", "owners": [], "pid": {"revision_id": 0, "type": "depid", "value": "25997"}, "status": "published"}, "_oai": {"id": "oai:nagoya.repo.nii.ac.jp:00025997"}, "item_10_biblio_info_6": {"attribute_name": "\u66f8\u8a8c\u60c5\u5831", "attribute_value_mlt": [{"bibliographicIssueDates": {"bibliographicIssueDate": "2018-04", "bibliographicIssueDateType": "Issued"}, "bibliographicIssueNumber": "4", "bibliographicPageEnd": "2534", "bibliographicPageStart": "2520", "bibliographicVolumeNumber": "123", "bibliographic_titles": [{"bibliographic_title": "Journal of Geophysical Research: Space Physics"}]}]}, "item_10_description_4": {"attribute_name": "\u6284\u9332", "attribute_value_mlt": [{"subitem_description": "We investigate long\u2010term variation of the very slow solar wind (VSSW), whose speed is less than 350 km/s, during the period between 1997 and 2015, that is, Cycles 23 and 24, using interplanetary scintillation measurements, which enable determination of the global distribution of the flow speed and the electron density fluctuation level \u0394Ne. We find that the occurrence rate of VSSW increases in the maximum phase of the solar cycle, and it was mostly associated with high \u0394Ne in Cycle 23. However, the VSSW is found to be more associated with low \u0394Ne in Cycle 24. This fact is consistent with an increased occurrence of the low\u2010density VSSW observed in situ in Cycle 24. These facts, which are considered to be a manifestation of weak solar activity in this cycle, suggest that the VSSW has become significantly rarefied in recent years. We identify the source region of the VSSW on the photosphere using a potential field analysis and examine the magnetic field properties of the VSSW source. We find that the low\u2010\u0394Ne VSSW is associated with a smaller expansion factor and possibly a slightly weaker photospheric field strength than the high\u2010\u0394Ne VSSW. The results obtained here may suggest that more open magnetic field areas producing the VSSW in Cycle 24 are formed in the quiet Sun region, which is associated with a lower mass flux supply into the corona, than those in Cycle 23.", "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\uff1a2018-10-26", "subitem_description_type": "Other"}]}, "item_10_publisher_32": {"attribute_name": "\u51fa\u7248\u8005", "attribute_value_mlt": [{"subitem_publisher": "Wiley"}]}, "item_10_relation_11": {"attribute_name": "DOI", "attribute_value_mlt": [{"subitem_relation_type_id": {"subitem_relation_type_id_text": "https://doi.org/10.1002/2017JA025014", "subitem_relation_type_select": "DOI"}}]}, "item_10_rights_12": {"attribute_name": "\u6a29\u5229", "attribute_value_mlt": [{"subitem_rights": "\u00a9 2018 American Geophysical Union "}]}, "item_10_select_15": {"attribute_name": "\u8457\u8005\u7248\u30d5\u30e9\u30b0", "attribute_value_mlt": [{"subitem_select_item": "publisher"}]}, "item_10_source_id_7": {"attribute_name": "ISSN", "attribute_value_mlt": [{"subitem_source_identifier": "21699380", "subitem_source_identifier_type": "ISSN"}]}, "item_creator": {"attribute_name": "\u8457\u8005", "attribute_type": "creator", "attribute_value_mlt": [{"creatorNames": [{"creatorName": "Tokumaru, Munetoshi"}], "nameIdentifiers": [{"nameIdentifier": "77213", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Shimoyama, Tomoya"}], "nameIdentifiers": [{"nameIdentifier": "77214", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Fujiki, Ken\u0027ichi"}], "nameIdentifiers": [{"nameIdentifier": "77215", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Hakamada, Kazuyuki"}], "nameIdentifiers": [{"nameIdentifier": "77216", "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": "2018-10-26"}], "displaytype": "detail", "download_preview_message": "", "file_order": 0, "filename": "Tokumaru_et_al-2018.pdf", "filesize": [{"value": "2.7 MB"}], "format": "application/pdf", "future_date_message": "", "is_thumbnail": false, "licensetype": "license_free", "mimetype": "application/pdf", "size": 2700000.0, "url": {"label": "Tokumaru_et_al-2018", "url": "https://nagoya.repo.nii.ac.jp/record/25997/files/Tokumaru_et_al-2018.pdf"}, "version_id": "2a5df11c-7187-4b12-a212-f9f0b849b6de"}]}, "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": "solar cycle variation", "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": "Rarefaction of the Very Slow (\u003c350 km/s) Solar Wind in Cycle 24 Compared With Cycle 23", "item_titles": {"attribute_name": "\u30bf\u30a4\u30c8\u30eb", "attribute_value_mlt": [{"subitem_title": "Rarefaction of the Very Slow (\u003c350 km/s) Solar Wind in Cycle 24 Compared With Cycle 23"}]}, "item_type_id": "10", "owner": "1", "path": ["879/880/881"], "permalink_uri": "http://hdl.handle.net/2237/00028202", "pubdate": {"attribute_name": "\u516c\u958b\u65e5", "attribute_value": "2018-05-23"}, "publish_date": "2018-05-23", "publish_status": "0", "recid": "25997", "relation": {}, "relation_version_is_last": true, "title": ["Rarefaction of the Very Slow (\u003c350 km/s) Solar Wind in Cycle 24 Compared With Cycle 23"], "weko_shared_id": null}