WEKO3
アイテム
{"_buckets": {"deposit": "45f9edab-1e2e-4c25-9cae-cfcb0cb5e78f"}, "_deposit": {"created_by": 3, "id": "9826", "owners": [3], "pid": {"revision_id": 0, "type": "depid", "value": "9826"}, "status": "published"}, "_oai": {"id": "oai:nifs-repository.repo.nii.ac.jp:00009826", "sets": ["32"]}, "author_link": ["59950", "59949", "59951"], "item_5_biblio_info_7": {"attribute_name": "書誌情報", "attribute_value_mlt": [{"bibliographicIssueDates": {"bibliographicIssueDate": "1994-11-01", "bibliographicIssueDateType": "Issued"}, "bibliographic_titles": [{}, {"bibliographic_title": "Research Report NIFS-Series", "bibliographic_titleLang": "en"}]}]}, "item_5_description_5": {"attribute_name": "抄録", "attribute_value_mlt": [{"subitem_description": "\"We performed a computer simulation of a magnetohydrodynamic dynamo in a rapidly rotating spherical shell. Extensive parameter runs are carried out changing the electrical resistivity. It is found that the total magnetic energy can grow more than ten times larger than the total kinetic energy of the convection motion when the resistivity is sufficiently small. When the resistivity is relatively large and the magnetic energy is comparable or smaller than the kinetic energy, the convection motion maintains its well-organized structure. However, when the resistivity is small and the magnetic energy becomes larger than the kinetic energy, the well-organized convection motion is highly disturbed. The generated magnetic field is organized as a set of flux tubes which can be divided into two categories. The magnetic field component parallel to the rotation axis tends to be confined inside the anticyclonic columnar convection cells. On the other hand, the component perpendicular to the rotation axis is confined outside the convection cell.\"", "subitem_description_type": "Abstract"}]}, "item_5_source_id_10": {"attribute_name": "ISSN", "attribute_value_mlt": [{"subitem_source_identifier": "0915-633X", "subitem_source_identifier_type": "ISSN"}]}, "item_5_text_25": {"attribute_name": "登録情報", "attribute_value_mlt": [{"subitem_text_value": "Made available in DSpace on 2010-02-05T10:17:21Z (GMT). No. of bitstreams: 0\n Previous issue date: 1994-11"}]}, "item_5_text_8": {"attribute_name": "報告書番号", "attribute_value_mlt": [{"subitem_text_value": "NIFS-320"}]}, "item_access_right": {"attribute_name": "アクセス権", "attribute_value_mlt": [{"subitem_access_right": "metadata only access", "subitem_access_right_uri": "http://purl.org/coar/access_right/c_14cb"}]}, "item_creator": {"attribute_name": "著者", "attribute_type": "creator", "attribute_value_mlt": [{"creatorNames": [{"creatorName": "\"Kageyama, A.", "creatorNameLang": "en"}], "nameIdentifiers": [{"nameIdentifier": "59949", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Sato, T.", "creatorNameLang": "en"}], "nameIdentifiers": [{"nameIdentifier": "59950", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "The, Complexity Simulation Group\"", "creatorNameLang": "en"}], "nameIdentifiers": [{"nameIdentifier": "59951", "nameIdentifierScheme": "WEKO"}]}]}, "item_keyword": {"attribute_name": "キーワード", "attribute_value_mlt": [{"subitem_subject": "MHD dynamo", "subitem_subject_language": "en", "subitem_subject_scheme": "Other"}, {"subitem_subject": "geomagnetic field", "subitem_subject_language": "en", "subitem_subject_scheme": "Other"}, {"subitem_subject": "solar magnetic field", "subitem_subject_language": "en", "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": "research report", "resourceuri": "http://purl.org/coar/resource_type/c_18ws"}]}, "item_title": "Computer Simulation of a Magnetohydrodynamic Dynamo II", "item_titles": {"attribute_name": "タイトル", "attribute_value_mlt": [{"subitem_title": "Computer Simulation of a Magnetohydrodynamic Dynamo II", "subitem_title_language": "en"}]}, "item_type_id": "5", "owner": "3", "path": ["32"], "permalink_uri": "http://hdl.handle.net/10655/2613", "pubdate": {"attribute_name": "公開日", "attribute_value": "2010-02-05"}, "publish_date": "2010-02-05", "publish_status": "0", "recid": "9826", "relation": {}, "relation_version_is_last": true, "title": ["Computer Simulation of a Magnetohydrodynamic Dynamo II"], "weko_shared_id": -1}
Computer Simulation of a Magnetohydrodynamic Dynamo II
http://hdl.handle.net/10655/2613
http://hdl.handle.net/10655/2613d20a9e80-fd6e-4e9b-aca0-b5f5a73cdb85
Item type | 研究報告書 / Research Paper(1) | |||||
---|---|---|---|---|---|---|
公開日 | 2010-02-05 | |||||
タイトル | ||||||
言語 | en | |||||
タイトル | Computer Simulation of a Magnetohydrodynamic Dynamo II | |||||
言語 | ||||||
言語 | eng | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | MHD dynamo | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | geomagnetic field | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | solar magnetic field | |||||
資源タイプ | ||||||
資源タイプ識別子 | http://purl.org/coar/resource_type/c_18ws | |||||
資源タイプ | research report | |||||
アクセス権 | ||||||
アクセス権 | metadata only access | |||||
アクセス権URI | http://purl.org/coar/access_right/c_14cb | |||||
著者 |
"Kageyama, A.
× "Kageyama, A.× Sato, T.× The, Complexity Simulation Group" |
|||||
抄録 | ||||||
内容記述タイプ | Abstract | |||||
内容記述 | "We performed a computer simulation of a magnetohydrodynamic dynamo in a rapidly rotating spherical shell. Extensive parameter runs are carried out changing the electrical resistivity. It is found that the total magnetic energy can grow more than ten times larger than the total kinetic energy of the convection motion when the resistivity is sufficiently small. When the resistivity is relatively large and the magnetic energy is comparable or smaller than the kinetic energy, the convection motion maintains its well-organized structure. However, when the resistivity is small and the magnetic energy becomes larger than the kinetic energy, the well-organized convection motion is highly disturbed. The generated magnetic field is organized as a set of flux tubes which can be divided into two categories. The magnetic field component parallel to the rotation axis tends to be confined inside the anticyclonic columnar convection cells. On the other hand, the component perpendicular to the rotation axis is confined outside the convection cell." | |||||
書誌情報 |
en : Research Report NIFS-Series 発行日 1994-11-01 |
|||||
報告書番号 | ||||||
NIFS-320 | ||||||
ISSN | ||||||
収録物識別子タイプ | ISSN | |||||
収録物識別子 | 0915-633X |