Coronal current sheet signatures during the 17 May 2002 CME-flare
Coronal current sheet signatures during the 17 May 2002 CME-flare
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DOI：
10.1051/0004-6361/200912229
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发表时间：
2009-11
影响因子：
6.5
通讯作者：
H. Aurass;F. Landini;G. Poletto
中科院分区：
文献类型：
--
作者：
H. Aurass;F. Landini;G. Poletto
上下文特征射电信号揭示的耀斑电流片与日冕紫外光和白色光观测的日冕物质抛射电流片之间的关系尚未得到分析。目标。我们的目的是建立与肢体耀斑和CS与CME，显然是耀斑后发展的CS之间的关系。我们使用2002年5月17日获得的独特数据集，其中包括射电和极紫外（XUV）观测结果。方法.光谱无线电诊断，紫外光谱技术，白色光日冕成像，（部分）无线电成像被用来说明CS之间的关系，并推断的物理参数的径向对齐的功能，在CME的后果发展。结果在耀斑期间，几种现象被解释为根据早期的工作，并参考常见的爆发性耀斑的情况下，作为证据的耀斑CSs在低日冕。这些是动态射电频谱中的漂移脉动结构，爆发的灯丝，扩张的日冕环，在形态上回忆起后来的白色光CME，并与早期报道的硬X射线源站点有关。在CME之后，紫外光谱使我们能够估计CS的温度和密度，在1.5 - 2.1 $R\odot $日心高度的间隔。然而，紫外线探测到的CS似乎只是存在于爆发通量绳下面的许多电流片之一。一个II型爆发后的CME无线电连续时间在较低的频率被认为是一个日冕冲击的射电签名激发在侧翼的CME。结论.结果表明，我们可以建立一个整体的情况下，CME解释的爆发拱廊横跨太阳的肢体，并通过多个CS连接到底层结构。最终，观测到的临边耀斑似乎是持续的CME的结果。
Context. The relation between current sheets (CSs) associated with flares, revealed by characteristic radio signatures, and current sheets associated with coronal mass ejections (CMEs), detected in coronal ultraviolet (UV) and white light data, has not been analyzed, yet. Aims. We aim at establishing the relationship between CSs associated with a limb flare and CSs associated with the CME that apparently develops after the flare. We use a unique data set, acquired on May 17, 2002, which includes radio and extreme ultraviolet (XUV) observations. Methods. Spectral radio diagnostics, UV spectroscopic techniques, white light coronograph imaging, and (partly) radio imaging are used to illustrate the relation between the CSs and to infer the physical parameters of the radially aligned features that develop in the aftermath of the CME. Results. During the flare, several phenomena are interpreted in accordance with earlier work and with reference to the common eruptive flare scenario as evidence of flare CSs in the low corona. These are drifting pulsating structures in dynamic radio spectra, an erupting filament, expanding coronal loops morphologically recalling the later white light CME, and associated with earlier reported hard X-ray source sites. In the aftermath of the CME, UV spectra allowed us to estimate the CS temperature and density, over the 1.5–2.1 $R_\odot$ interval of heliocentric altitudes. The UV detected CS, however, appears to be only one of many current sheets that exist underneath the erupting flux rope. A type II burst following the CME radio continuum in time at lower frequencies is considered as the radio signature of a coronal shock excited at the flank of the CME. Conclusions. The results show that we can build an overall scenario where the CME is interpreted in terms of an erupting arcade crossing the limb of the Sun and connected to underlying structures via multiple CSs. Eventually, the observed limb flare seems to be a consequence of the ongoing CME.