论文标题
用喷气
Identifying the energy release site in a Solar microflare with a jet
论文作者
论文摘要
太阳轨道和帕克太阳能探测任务的主要科学问题之一涉及了解下太阳能电晕中的电子如何加速以及它们随后如何访问行星际空间。我们旨在研究电子加速度和能量释放位点以及在Sol2021-02-02-18T18：05事件的情况下加速电子访问行星际空间的方式，A GOOS A8类小型与冠状射流相关。这项研究利用了三个不同的有利位点，即太阳能轨道，立体声A和地球，观察结果从无线电到X射线。多波长的时间分析与太阳轨道/stix（用于成像X射线的光谱仪/望远镜）结合使用UV/EUV图像和X射线光谱，以研究不同耀斑阶段观察到的发射的起源。正在调查的事件满足了与射流和无线电III爆发一致的电子加速的经典图片。该微叶片具有突出的硬X射线非热发射，至少为10 keV和光谱，对于光谱指数为2.9的微叶片比平常要困难得多。从地球的有利位置可以看到肢体附近的微叶片，从EUV中的耀斑环上方揭示了冠状能释放位点，从Stix Spectromoscic分析中，该位点被证明是热的（在耀斑的温度大致相同的情况下）。此外，随着时间的流逝（约30 km/s），该区域正朝着更高的高度转向。在耀斑期间，同一区域在空间上与冠状射流的起源一致。我们得出的结论是，在环上观察到的能量释放位点对应于电子加速度位点，证实了互换重新连接是在低谷线上的颗粒加速度的可行候选者，该候选是通向行星际空间的野外线。
One of the main science questions of the Solar Orbiter and Parker Solar Probe missions deals with understanding how electrons in the lower solar corona are accelerated and how they subsequently access interplanetary space. We aim to investigate the electron acceleration and energy release sites as well as the manner in which accelerated electrons access the interplanetary space in the case of the SOL2021-02-18T18:05 event, a GOES A8 class microflare associated with a coronal jet. This study takes advantage of three different vantage points, Solar Orbiter, STEREO-A, and Earth, with observations ranging from radio to X-ray. Multi-wavelength timing analysis combined with UV/EUV imagery and X-ray spectroscopy by Solar Orbiter/STIX (Spectrometer/Telescope for Imaging X-rays) is used to investigate the origin of the observed emission during different flare phases. The event under investigation satisfies the classical picture of the onset time of the acceleration of electrons coinciding with the jet and the radio type III bursts. This microflare features prominent hard X-ray nonthermal emission down to at least 10 keV and a spectrum that is much harder than usual for a microflare with a spectral index of 2.9. From Earth's vantage point, the microflare is seen near the limb, revealing the coronal energy release site above the flare loop in EUV, which, from STIX spectroscopic analysis, turns out to be hot (at roughly the same temperature of the flare). Moreover, this region is moving toward higher altitudes over time (about 30 km/s). During the flare, the same region spatially coincides with the origin of the coronal jet. We conclude that the energy release site observed above-the-loop corresponds to the electron acceleration site, corroborating that interchange reconnection is a viable candidate for particle acceleration in the low corona on field lines open to interplanetary space.
