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Magnetic Structure of a Composite Solar Microwave Burst
http://hdl.handle.net/2237/00028306
http://hdl.handle.net/2237/00028306ae8e164a-b9c9-4950-8149-db1238c7034a
名前 / ファイル | ライセンス | アクション |
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Item type | 学術雑誌論文 / Journal Article(1) | |||||
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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× White, Stephen M.× Liu, Chang× Kliem, Bernhard× Masuda, Satoshi |
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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 |
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著者版フラグ | ||||||
値 | publisher |