日本語
 
Help Privacy Policy ポリシー/免責事項
  詳細検索ブラウズ

アイテム詳細

登録内容を編集ファイル形式で保存
一時保存へ追加
 タグ情報を表示リリース履歴を表示詳細要約
  Properties of a Small-scale Short-duration Solar Eruption with a Driven Shock

Ying, B., Feng, L., Lu, L., Zhang, J., Magdalenic, J., Su, Y., Su, Y., & Gan, W. (2018). Properties of a Small-scale Short-duration Solar Eruption with a Driven Shock. The Astrophysical Journal, 856(1):. doi:10.3847/1538-4357/aaadaf.

Item is

 

表示: 全項目 非表示: 全項目

基本情報

表示: 非表示:
アイテムのパーマリンク: https://hdl.handle.net/21.11116/0000-0002-1873-2 版のパーマリンク: https://hdl.handle.net/21.11116/0000-0002-1874-1
資料種別: 学術論文

ファイル

表示: ファイル

関連URL

表示:

作成者

表示:
非表示:
 作成者:
Ying, Beili1, 著者
Feng, Li, 著者
Lu, Lei, 著者
Zhang, Jie, 著者
Magdalenic, Jasmina, 著者
Su, Yingna, 著者
Su, Yang, 著者
Gan, Weiqun, 著者
所属:
1Department Sun and Heliosphere, Max Planck Institute for Solar System Research, Max Planck Society, Justus-von-Liebig-Weg 3, 37077 Göttingen, DE, ou_1832289              

内容説明

表示:
非表示:
キーワード: shock waves; Sun: corona; Sun: coronal mass ejections (CMEs) ; Sun: flares
 要旨: Large-scale solar eruptions have been extensively explored over many years. However, the properties of small-scale events with associated shocks have rarely been investigated. We present analyses of a small-scale, short-duration event originating from a small region. The impulsive phase of the M1.9-class flare lasted only four minutes. The kinematic evolution of the CME hot channel reveals some exceptional characteristics, including a very short duration of the main acceleration phase (<2 minutes), a rather high maximal acceleration rate (~50 km s−2), and peak velocity (~1800 km s−1). The fast and impulsive kinematics subsequently results in a piston-driven shock related to a metric type II radio burst with a high starting frequency of ~320 MHz of the fundamental band. The type II source is formed at a low height of below 1.1 R⊙ less than ~2 minutes after the onset of the main acceleration phase. Through the band-split of the type II burst, the shock compression ratio decreases from 2.2 to 1.3, and the magnetic field strength of the shock upstream region decreases from 13 to 0.5 Gauss at heights of 1.1–2.3 R⊙. We find that the CME (~4 × 1030 erg) and flare (~1.6 × 1030 erg) consume similar amounts of magnetic energy. The same conclusion for large-scale eruptions implies that small- and large-scale events possibly share a similar relationship between CMEs and flares. The kinematic particularities of this event are possibly related to the small footpoint-separation distance of the associated magnetic flux rope, as predicted by the Erupting Flux Rope model.

資料詳細

表示:
非表示:
言語: eng - English
 日付: 2018-09-172018
 出版の状態: オンラインで出版済み
 ページ: -
 出版情報: -
 目次: -
 査読: 査読あり
 識別子（DOI, ISBNなど）: DOI: 10.3847/1538-4357/aaadaf
 学位: -

関連イベント

表示:

訴訟

表示:

Project information

表示:

出版物 1

表示:
非表示:
出版物名: The Astrophysical Journal
種別: 学術雑誌
 著者・編者:
所属:
出版社, 出版地: Bristol; Vienna : IOP Publishing; IAEA
ページ: - 巻号: 856 (1) 通巻号: 24 開始・終了ページ: - 識別子（ISBN, ISSN, DOIなど）: ISSN: 0004-637X
CoNE: https://pure.mpg.de/cone/journals/resource/954922828215_3