{"_buckets": {"deposit": "8f9e88bf-7e92-49c0-9eef-061daf5d2168"}, "_deposit": {"created_by": 17, "id": "2001525", "owner": "17", "owners": [17], "owners_ext": {"displayname": "図書情報係", "username": "repository"}, "pid": {"revision_id": 0, "type": "depid", "value": "2001525"}, "status": "published"}, "_oai": {"id": "oai:nagoya.repo.nii.ac.jp:02001525", "sets": ["881"]}, "author_link": [], "item_1615768549627": {"attribute_name": "出版タイプ", "attribute_value_mlt": [{"subitem_version_resource": "http://purl.org/coar/version/c_970fb48d4fbd8a85", "subitem_version_type": "VoR"}]}, "item_1629683748249": {"attribute_name": "日付", "attribute_value_mlt": [{"subitem_date_issued_datetime": "2021-10-15", "subitem_date_issued_type": "Available"}]}, "item_9_biblio_info_6": {"attribute_name": "書誌情報", "attribute_value_mlt": [{"bibliographicIssueDates": {"bibliographicIssueDate": "2021-03-15", "bibliographicIssueDateType": "Issued"}, "bibliographicIssueNumber": "2", "bibliographicPageStart": "155", "bibliographicVolumeNumber": "909", "bibliographic_titles": [{"bibliographic_title": "The Astrophysical Journal", "bibliographic_titleLang": "en"}]}]}, "item_9_description_4": {"attribute_name": "内容記述", "attribute_value_mlt": [{"subitem_description": "Solar flares and plasma eruptions are sudden releases of magnetic energy stored in the plasma atmosphere. To understand the physical mechanisms governing their occurrences, three-dimensional magnetic fields from the photosphere up to the corona must be studied. The solar photospheric magnetic fields are observable, whereas the coronal magnetic fields cannot be measured. One method for inferring coronal magnetic fields is performing data-driven simulations, which involves time-series observational data of the photospheric magnetic fields with the bottom boundary of magnetohydrodynamic simulations. We developed a data-driven method in which temporal evolutions of the observational vector magnetic field can be reproduced at the bottom boundary in the simulation by introducing an inverted velocity field. This velocity field is obtained by inversely solving the induction equation and applying an appropriate gauge transformation. Using this method, we performed a data-driven simulation of successive small eruptions observed by the Solar Dynamics Observatory and the Solar Magnetic Activity Telescope in 2017 November. The simulation well reproduced the converging motion between opposite-polarity magnetic patches, demonstrating successive formation and eruptions of helical flux ropes.", "subitem_description_language": "en", "subitem_description_type": "Abstract"}]}, "item_9_publisher_32": {"attribute_name": "出版者", "attribute_value_mlt": [{"subitem_publisher": "IOP publishing", "subitem_publisher_language": "en"}]}, "item_9_relation_43": {"attribute_name": "関連情報", "attribute_value_mlt": [{"subitem_relation_type": "isVersionOf", "subitem_relation_type_id": {"subitem_relation_type_id_text": "https://doi.org/10.3847/1538-4357/abe414", "subitem_relation_type_select": "DOI"}}]}, "item_9_rights_12": {"attribute_name": "権利", "attribute_value_mlt": [{"subitem_rights": "© 2021. The American Astronomical Society", "subitem_rights_language": "en"}]}, "item_9_source_id_7": {"attribute_name": "収録物識別子", "attribute_value_mlt": [{"subitem_source_identifier": "0004-637X", "subitem_source_identifier_type": "PISSN"}]}, "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": "Kaneko, Takafumi", "creatorNameLang": "en"}]}, {"creatorNames": [{"creatorName": "Park, Sung-Hong", "creatorNameLang": "en"}]}, {"creatorNames": [{"creatorName": "Kusano, Kanya", "creatorNameLang": "en"}]}]}, "item_files": {"attribute_name": "ファイル情報", "attribute_type": "file", "attribute_value_mlt": [{"accessrole": "open_access", "date": [{"dateType": "Available", "dateValue": "2021-10-15"}], "displaytype": "detail", "download_preview_message": "", "file_order": 0, "filename": "Kaneko_2021_ApJ_909_155.pdf", "filesize": [{"value": "2 MB"}], "format": "application/pdf", "future_date_message": "", "is_thumbnail": false, "mimetype": "application/pdf", "size": 2000000.0, "url": {"objectType": "fulltext", "url": "https://nagoya.repo.nii.ac.jp/record/2001525/files/Kaneko_2021_ApJ_909_155.pdf"}, "version_id": "a289463f-792f-4104-9335-573ed0029bcf"}]}, "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": "Data-driven MHD Simulation of Successive Solar Plasma Eruptions", "item_titles": {"attribute_name": "タイトル", "attribute_value_mlt": [{"subitem_title": "Data-driven MHD Simulation of Successive Solar Plasma Eruptions", "subitem_title_language": "en"}]}, "item_type_id": "40001", "owner": "17", "path": ["881"], "permalink_uri": "http://hdl.handle.net/2237/0002001525", "pubdate": {"attribute_name": "PubDate", "attribute_value": "2021-10-15"}, "publish_date": "2021-10-15", "publish_status": "0", "recid": "2001525", "relation": {}, "relation_version_is_last": true, "title": ["Data-driven MHD Simulation of Successive Solar Plasma Eruptions"], "weko_shared_id": -1}