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  1. F300 宇宙地球環境研究所
  2. F300a 雑誌掲載論文
  3. 学術雑誌

Magnetic Structure of a Composite Solar Microwave Burst

http://hdl.handle.net/2237/00028306
http://hdl.handle.net/2237/00028306
ae8e164a-b9c9-4950-8149-db1238c7034a
名前 / ファイル ライセンス アクション
Lee_2018_ApJ_856_70.pdf Lee_2018_ApJ_856_70 (5.5 MB)
Item type 学術雑誌論文 / Journal Article(1)
公開日 2018-06-13
タイトル
タイトル Magnetic Structure of a Composite Solar Microwave Burst
言語 en
著者 Lee, Jeongwoo

× Lee, Jeongwoo

WEKO 78289

en Lee, Jeongwoo

Search repository
White, Stephen M.

× White, Stephen M.

WEKO 78290

en White, Stephen M.

Search repository
Liu, Chang

× Liu, Chang

WEKO 78291

en Liu, Chang

Search repository
Kliem, Bernhard

× Kliem, Bernhard

WEKO 78292

en Kliem, Bernhard

Search repository
Masuda, Satoshi

× Masuda, Satoshi

WEKO 78293

en Masuda, Satoshi

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 © 2018. 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: coronal mass ejections (CMEs)
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 Sun: radio radiation
キーワード
主題Scheme Other
主題 Sun: UV radiation
抄録
内容記述 A composite flare consisting of an impulsive flare SOL2015-06-21T01:42 (GOES class M2.0) and a more gradual, long-duration flare SOL2015-06-21T02:36 (M2.6) from NOAA Active Region 12371, is studied using observations with the Nobeyama Radioheliograph (NoRH) and the Solar Dynamics Observatory (SDO). While composite flares are defined by their characteristic time profiles, in this paper we present imaging observations that demonstrate the spatial relationship of the two flares and allow us to address the nature of the evolution of a composite event. The NoRH maps show that the first flare is confined not only in time, but also in space, as evidenced by the stagnation of ribbon separation and the stationarity of the microwave source. The NoRH also detected another microwave source during the second flare, emerging from a different location where thermal plasma is so depleted that accelerated electrons could survive longer against Coulomb collisional loss. The AIA 131 Å images show that a sigmoidal EUV hot channel developed after the first flare and erupted before the second flare. We suggest that this eruption removed the high-lying flux to let the separatrix dome underneath reconnect with neighboring flux and the second microwave burst follow. This scenario explains how the first microwave burst is related to the much-delayed second microwave burst in this composite event.
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/aaadbc
ISSN
収録物識別子タイプ EISSN
収録物識別子 1538-4357
書誌情報 en : The Astrophysical Journal

巻 856, 号 1, p. 70, 発行日 2018-03-26
著者版フラグ
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