ログイン
言語:

WEKO3

  • トップ
  • ランキング
To
lat lon distance
To

Field does not validate



インデックスリンク

インデックスツリー

メールアドレスを入力してください。

WEKO

One fine body…

WEKO

One fine body…

アイテム

{"_buckets": {"deposit": "4183d3c6-6373-4698-b140-b4950814dd39"}, "_deposit": {"id": "24557", "owners": [], "pid": {"revision_id": 0, "type": "depid", "value": "24557"}, "status": "published"}, "_oai": {"id": "oai:nagoya.repo.nii.ac.jp:00024557", "sets": ["881"]}, "author_link": ["72698", "72699", "72700", "72701"], "item_10_biblio_info_6": {"attribute_name": "書誌情報", "attribute_value_mlt": [{"bibliographicIssueDates": {"bibliographicIssueDate": "2017-04", "bibliographicIssueDateType": "Issued"}, "bibliographicIssueNumber": "2", "bibliographicPageEnd": "134", "bibliographicPageStart": "134", "bibliographicVolumeNumber": "838", "bibliographic_titles": [{"bibliographic_title": "The Astrophysical Journal", "bibliographic_titleLang": "en"}]}]}, "item_10_description_4": {"attribute_name": "抄録", "attribute_value_mlt": [{"subitem_description": "The solar magnetic field in a flare-producing active region (AR) is much more complicated than theoretical models, which assume a very simple magnetic field structure. The X1.0 flare, which occurred in AR 12192 on 2014 October 25, showed a complicated three-ribbon structure. To clarify the trigger process of the flare and to evaluate the applicability of a simple theoretical model, we analyzed the data from Hinode/Solar Optical Telescope and the Solar Dynamics Observatory/Helioseismic and Magnetic Imager, Atmospheric Imaging Assembly. We investigated the spatio-temporal correlation between the magnetic field structures, especially the non-potentiality of the horizontal field, and the bright structures in the solar atmosphere. As a result, we determined that the western side of the positive polarity, which is intruding on a negative polarity region, is the location where the flare was triggered. This is due to the fact that the sign of the magnetic shear in that region was opposite that of the major shear of the AR, and the significant brightenings were observed over the polarity inversion line (PIL) in that region before flare onset. These features are consistent with the recently proposed flare-trigger model that suggests that small reversed shear (RS) magnetic disturbances can trigger solar flares. Moreover, we found that the RS field was located slightly off the flaring PIL, contrary to the theoretical prediction. We discuss the possibility of an extension of the RS model based on an extra numerical simulation. Our result suggests that the RS field has a certain flexibility for displacement from a highly sheared PIL, and that the RS field triggers more flares than we expected.", "subitem_description_language": "en", "subitem_description_type": "Abstract"}]}, "item_10_identifier_60": {"attribute_name": "URI", "attribute_value_mlt": [{"subitem_identifier_type": "DOI", "subitem_identifier_uri": "https://doi.org/10.3847/1538-4357/aa6682"}, {"subitem_identifier_type": "HDL", "subitem_identifier_uri": "http://hdl.handle.net/2237/26775"}]}, "item_10_publisher_32": {"attribute_name": "出版者", "attribute_value_mlt": [{"subitem_publisher": "IOP publishing", "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/10.3847/1538-4357/aa6682", "subitem_relation_type_select": "DOI"}}]}, "item_10_rights_12": {"attribute_name": "権利", "attribute_value_mlt": [{"subitem_rights": "© 2017 The American Astronomical Society", "subitem_rights_language": "en"}]}, "item_10_select_15": {"attribute_name": "著者版フラグ", "attribute_value_mlt": [{"subitem_select_item": "publisher"}]}, "item_10_source_id_7": {"attribute_name": "ISSN", "attribute_value_mlt": [{"subitem_source_identifier": "0004-637X", "subitem_source_identifier_type": "PISSN"}]}, "item_1615787544753": {"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_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": "Bamba, Yumi", "creatorNameLang": "en"}], "nameIdentifiers": [{"nameIdentifier": "72698", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Inoue, Satoshi", "creatorNameLang": "en"}], "nameIdentifiers": [{"nameIdentifier": "72699", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Kusano, Kanya", "creatorNameLang": "en"}], "nameIdentifiers": [{"nameIdentifier": "72700", "nameIdentifierScheme": "WEKO"}]}, {"creatorNames": [{"creatorName": "Shiota, Daikou", "creatorNameLang": "en"}], "nameIdentifiers": [{"nameIdentifier": "72701", "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": "2018-02-22"}], "displaytype": "detail", "download_preview_message": "", "file_order": 0, "filename": "Bamba_2017_ApJ_838_134.pdf", "filesize": [{"value": "10.6 MB"}], "format": "application/pdf", "future_date_message": "", "is_thumbnail": false, "licensetype": "license_note", "mimetype": "application/pdf", "size": 10600000.0, "url": {"label": "Bamba_2017_ApJ_838_134.pdf", "objectType": "fulltext", "url": "https://nagoya.repo.nii.ac.jp/record/24557/files/Bamba_2017_ApJ_838_134.pdf"}, "version_id": "600e7b89-0e24-493f-bc7d-f65fefd2cd71"}]}, "item_keyword": {"attribute_name": "キーワード", "attribute_value_mlt": [{"subitem_subject": "Sun: activity", "subitem_subject_scheme": "Other"}, {"subitem_subject": "Sun: flares", "subitem_subject_scheme": "Other"}, {"subitem_subject": "Sun: magnetic fields", "subitem_subject_scheme": "Other"}, {"subitem_subject": "sunspots", "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": "Triggering Process of the X1.0 Three-ribbon Flare in the Great Active Region NOAA 12192", "item_titles": {"attribute_name": "タイトル", "attribute_value_mlt": [{"subitem_title": "Triggering Process of the X1.0 Three-ribbon Flare in the Great Active Region NOAA 12192", "subitem_title_language": "en"}]}, "item_type_id": "10", "owner": "1", "path": ["881"], "permalink_uri": "http://hdl.handle.net/2237/26775", "pubdate": {"attribute_name": "PubDate", "attribute_value": "2017-07-05"}, "publish_date": "2017-07-05", "publish_status": "0", "recid": "24557", "relation": {}, "relation_version_is_last": true, "title": ["Triggering Process of the X1.0 Three-ribbon Flare in the Great Active Region NOAA 12192"], "weko_shared_id": -1}
  1. F300 宇宙地球環境研究所
  2. F300a 雑誌掲載論文
  3. 学術雑誌

Triggering Process of the X1.0 Three-ribbon Flare in the Great Active Region NOAA 12192

http://hdl.handle.net/2237/26775
http://hdl.handle.net/2237/26775
746d3f46-ead0-41c9-a415-f7dcf00ce069
名前 / ファイル ライセンス アクション
Bamba_2017_ApJ_838_134.pdf Bamba_2017_ApJ_838_134.pdf (10.6 MB)
Item type 学術雑誌論文 / Journal Article(1)
公開日 2017-07-05
タイトル
タイトル Triggering Process of the X1.0 Three-ribbon Flare in the Great Active Region NOAA 12192
言語 en
著者 Bamba, Yumi

× Bamba, Yumi

WEKO 72698

en Bamba, Yumi

Search repository
Inoue, Satoshi

× Inoue, Satoshi

WEKO 72699

en Inoue, Satoshi

Search repository
Kusano, Kanya

× Kusano, Kanya

WEKO 72700

en Kusano, Kanya

Search repository
Shiota, Daikou

× Shiota, Daikou

WEKO 72701

en Shiota, Daikou

Search repository
アクセス権
アクセス権 open access
アクセス権URI http://purl.org/coar/access_right/c_abf2
権利
言語 en
権利情報 © 2017 The American Astronomical Society
キーワード
主題Scheme Other
主題 Sun: activity
キーワード
主題Scheme Other
主題 Sun: flares
キーワード
主題Scheme Other
主題 Sun: magnetic fields
キーワード
主題Scheme Other
主題 sunspots
抄録
内容記述 The solar magnetic field in a flare-producing active region (AR) is much more complicated than theoretical models, which assume a very simple magnetic field structure. The X1.0 flare, which occurred in AR 12192 on 2014 October 25, showed a complicated three-ribbon structure. To clarify the trigger process of the flare and to evaluate the applicability of a simple theoretical model, we analyzed the data from Hinode/Solar Optical Telescope and the Solar Dynamics Observatory/Helioseismic and Magnetic Imager, Atmospheric Imaging Assembly. We investigated the spatio-temporal correlation between the magnetic field structures, especially the non-potentiality of the horizontal field, and the bright structures in the solar atmosphere. As a result, we determined that the western side of the positive polarity, which is intruding on a negative polarity region, is the location where the flare was triggered. This is due to the fact that the sign of the magnetic shear in that region was opposite that of the major shear of the AR, and the significant brightenings were observed over the polarity inversion line (PIL) in that region before flare onset. These features are consistent with the recently proposed flare-trigger model that suggests that small reversed shear (RS) magnetic disturbances can trigger solar flares. Moreover, we found that the RS field was located slightly off the flaring PIL, contrary to the theoretical prediction. We discuss the possibility of an extension of the RS model based on an extra numerical simulation. Our result suggests that the RS field has a certain flexibility for displacement from a highly sheared PIL, and that the RS field triggers more flares than we expected.
言語 en
内容記述タイプ Abstract
出版者
言語 en
出版者 IOP publishing
言語
言語 eng
資源タイプ
資源タイプresource http://purl.org/coar/resource_type/c_6501
タイプ journal article
出版タイプ
出版タイプ VoR
出版タイプResource http://purl.org/coar/version/c_970fb48d4fbd8a85
DOI
関連タイプ isVersionOf
識別子タイプ DOI
関連識別子 https://doi.org/10.3847/1538-4357/aa6682
ISSN
収録物識別子タイプ PISSN
収録物識別子 0004-637X
書誌情報 en : The Astrophysical Journal

巻 838, 号 2, p. 134-134, 発行日 2017-04
著者版フラグ
値 publisher
URI
識別子 https://doi.org/10.3847/1538-4357/aa6682
識別子タイプ DOI
URI
識別子 http://hdl.handle.net/2237/26775
識別子タイプ HDL
戻る
0
views
See details
Views

Versions

Ver.1 2021-03-01 14:00:25.750213
Show All versions

Share

Mendeley Twitter Facebook Print Addthis

Cite as

エクスポート

OAI-PMH
  • OAI-PMH JPCOAR
  • OAI-PMH DublinCore
  • OAI-PMH DDI
Other Formats
  • JSON
  • BIBTEX

Confirm


Powered by WEKO3


Powered by WEKO3