Evidence of a blast shock wave formation in a "CME streamer" interaction

被引：12

作者：

Eselevich, V. G. ^{[1
]}

Eselevich, M. V. ^{[1
]}

Sadykov, V. M. ^{[2
,3
]}

Zimovets, I. V. ^{[2
]}

机构：

[1] Russian Acad Sci, Inst Solar Terr Phys, Siberian Div, Irkutsk 664033, Russia

[2] Russian Acad Sci, Space Res Inst IKI, Moscow 117997, Russia

[3] State Univ, Moscow Inst Phys & Technol, Dolgoprudnyi 141700, Russia

来源：

ADVANCES IN SPACE RESEARCH | 2015年 / 56卷 / 12期

基金：

俄罗斯基础研究基金会;

关键词：

Solar flare; Coronal mass ejection; Shock wave; Type II radio burst; CORONAL MASS EJECTIONS; II RADIO-BURSTS; SPATIALLY-RESOLVED OBSERVATIONS; X-RAY; ORIGIN; KINEMATICS;

D O I：

10.1016/j.asr.2015.03.041

中图分类号：

V [航空、航天];

学科分类号：

08 ; 0825 ;

摘要：

Analysis of the solar event on 16 February 2011 (SOL2011-02-16T14:19) allows to classify it as an "impulsive" coronal mass ejection (CME) event. It is argued that the observed deviation of a streamer ray from its pre-event state and generation of a metric type II radio burst in this event was a result of a "CME-streamer" interaction in the lower corona (r less than or similar to 1.5 R-circle dot). Most probably, it was a consequence of an impulsive action of a compressed magnetic field to the streamer. This compression of the coronal magnetic field was due to a moving and expanding magnetic flux rope, which was a core of the CME. The estimated radial speed of the type II burst sources was significantly (approximate to 2-8 times) larger than the radial speed of the erupting flux rope, and it decreased rapidly with time. This indicates that during the "CME streamer" interaction a blast shock wave could be excited and propagated along the streamer. (C) 2015 COSPAR. Published by Elsevier Ltd. All rights reserved.

引用

页码：2793 / 2803

页数：11

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