2005年5月13日太阳活动区的爆发
The Eruption from a Sigmoidal Solar Active Region on 2005 May 13
摘要：
本文介绍了2005年5月13日起源于双极活动区NOAA 10759的M8.0耀斑及其相关快晕CME的多波长研究。源活动区在TRACE 171 A通道以及SXI软X射线图像上具有明显的S形结构，并且我们主要关注S形喷发的详细过程，这一过程由Halpha，WL，EUV/UV，射电和硬X射线（HXRs）等多波长数据证明。最重要的发现是耀斑增亮开始于活动区核心，早于磁绳上升运动。这个时间清楚地解决了一个主要的问题，在磁喷发发病的S形，即，是否爆发是由内部系绳切割，让通量绳上升向上或通量绳上升，由于失去平衡，后来引起系绳切割下面it. Our高的时间节奏SXI和Halpha数据显示，第一种情况是相关的喷发。作为其他主要的发现，我们有RHESSI HXR图像显示的变化HXR源从一个有限的足点结构到一个细长的带状结构后，耀斑最大，我们涉及到S形到拱廊演变。射电动力学谱显示，在S型扩张时，HXR存在II型前兆，在耀斑上升阶段，HXR存在漂移脉动结构。最后，II型和III型爆发被认为是在最大的HXR发射的时间，同时与最大的重联率来自耀斑带状运动在紫外线。我们解释这些不同的观察到的属性与失控的系绳切割模型提出的Moore等人。在2001年。
英文摘要：
This paper presents a multiwavelength study of the M8.0 flare and its associated fast halo CME that originated from a bipolar active region NOAA 10759 on 2005 May 13. The source active region has a conspicuous sigmoid structure at TRACE 171 A channel as well as in the SXI soft X-ray images, and we mainly concern ourselves with the detailed process of the sigmoid eruption as evidenced by the multiwavelength data ranging from Halpha, WL, EUV/UV, radio, and hard X-rays (HXRs). The most important finding is that the flare brightening starts in the core of the active region earlier than that of the rising motion of the flux rope. This timing clearly addresses one of the main issues in the magnetic eruption onset of sigmoid, namely, whether the eruption is initiated by an internal tether-cutting to allow the flux rope to rise upward or a flux rope rises due to a loss of equilibrium to later induce tether cutting below it. Our high time cadence SXI and Halpha data shows that the first scenario is relevant to this eruption. As other major findings, we have the RHESSI HXR images showing a change of the HXR source from a confined footpoint structure to an elongated ribbon-like structure after the flare maximum, which we relate to the sigmoid-to-arcade evolution. Radio dynamic spectrum shows a type II precursor that occurred at the time of expansion of the sigmoid and a drifting pulsating structure in the flare rising phase in HXR. Finally type II and III bursts are seen at the time of maximum HXR emission, simultaneous with the maximum reconnection rate derived from the flare ribbon motion in UV. We interpret these various observed properties with the runaway tether-cutting model proposed by Moore et al. in 2001.
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