Electron Acceleration and Jet-facilitated Escape in an M-class Solar Flare on 2002 August 19
Electron Acceleration and Jet-facilitated Escape in an M-class Solar Flare on 2002 August 19
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DOI：
10.3847/1538-4357/aacefe
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发表时间：
2018-06
期刊：
影响因子：
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通讯作者：
L. Glesener;G. Fleishman
中科院分区：
文献类型：
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作者：
L. Glesener;G. Fleishman
准直等离子体的突然喷流来自太阳上的许多位置，包括活动区域。磁场沿着喷流的出现通常是向行星际空间开放的，为任何耀斑加速的电子提供了一条清晰的“逃逸路线”，使喷流成为研究粒子加速和瞬态日光层事件的太阳源的有利可图的目标。韧致辐射硬X射线（HXR）原则上可以追踪沿着喷流路径逃逸的加速电子，但由于日冕的低密度，逃逸电子束的测量通常很困难。在这项工作中，我们增加了HXR观测与回旋同步辐射在微波中观察到的，以及极紫外（EUV）的发射和建模调查耀斑加速电子在日冕喷流。HXR和微波数据分别来自Rheven Ramaty高能太阳光谱成像仪（RHESSI）和欧文斯谷太阳能电池阵列（OVSA），对电子光谱和位置提供了补充性的见解，包括射流本身中加速电子的存在。来自Konus-Wind仪器的高时间分辨率HXR数据表明电子加速时间尺度为1秒或更短。我们使用太阳和日光层天文台（SOHO）/迈克尔逊多普勒成像仪（MDI），过渡区和日冕探测器（TRACE），RHESSI和OVSA数据作为约束条件，在GX模拟器框架中模拟高能电子分布。其结果是一个模拟的分布，由测量信息和约束，加速电子，因为他们逃离太阳。结合检测微波回旋同步辐射从一个开放的，而不是封闭的，磁配置，与现实的3D建模磁图，EUV和X射线发射的约束，我们得到了最严格的限制，以日期内的加速电子太阳射流。
Sudden jets of collimated plasma arise from many locations on the Sun, including active regions. The magnetic field along which a jet emerges is often open to interplanetary space, offering a clear “escape route” for any flare-accelerated electrons, making jets lucrative targets for studying particle acceleration and the solar sources of transient heliospheric events. Bremsstrahlung hard X-rays (HXRs) could, in principle, trace the accelerated electrons that escape along the paths of the jets, but measurements of the escaping electron beams are customarily difficult due to the low densities of the corona. In this work, we augment HXR observations with gyrosynchrotron emission observed in microwaves, as well as extreme ultraviolet (EUV) emission and modeling to investigate flare-accelerated electrons in a coronal jet. HXR and microwave data from the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) and the Owens Valley Solar Array (OVSA), respectively, give complementary insight into electron spectra and locations, including the presence of accelerated electrons in the jet itself. High-time-resolution HXR data from the Konus-Wind instrument suggest electron acceleration timescales on the order of 1 s or shorter. We model the energetic electron distributions in the GX Simulator framework using the Solar and Heliospheric Observatory (SOHO)/Michelson Doppler Imager (MDI), the Transition Region and Coronal Explorer (TRACE), RHESSI, and OVSA data as constraints. The result is a modeled distribution, informed and constrained by measurements, of accelerated electrons as they escape the Sun. Combining the detection of microwave gyrosynchrotron emission from an open, rather than closed, magnetic configuration, with realistic 3D modeling constrained by magnetograms, EUV, and X-ray emission, we obtain the most stringent constraints to date on the accelerated electrons within a solar jet.