太阳-C/EUVST 短波长相机观测到的耀斑前和活动区等离子体流动及结构
Pre-flare and active region plasma flows and structure seen by the short wavelength camera on SOLAR-C/EUVST
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中文总结 AI 辅助
研究太阳耀斑触发和日冕加热机制，通过对太阳-C/EUVST 短波长相机正向建模并与前代 EIS 比较，发现其能分辨通量管、捕捉速度梯度，精度优于 1km/s，有望直接观测耀斑触发相关过程并确定活动区环结构。
中文摘要 AI 辅助
触发太阳耀斑和驱动日冕加热的机制发生在小空间尺度和短时间尺度的宽温度范围内，难以用现有仪器观测。即将在 2020 年代末发射的太阳-C 任务，其高通量极紫外光谱望远镜（EUVST）将提供前所未有的等离子体诊断能力。本文对光谱仪短波长相机及其对三维磁流体动力学模拟的耀斑前活动区中对数 T~6.2 日冕等离子体的响应进行了正向建模，并与日之出卫星上的前代 EUV 成像光谱仪（EIS）性能作比较。结果表明，太阳-C/EUVST 能分辨日之出/EIS 无法分辨的活动区环中单个通量管，能捕捉相邻上升和下降等离子体间的急剧速度梯度，活动区中多普勒速度测量精度将优于 1km/s，有望直接观测与耀斑触发相关的过程，确定活动区环是由少数股还是磁重联诱导的纳米耀斑加热模型预测的数百股组成。
英文摘要
The mechanisms triggering solar flares and driving coronal heating occur across wide temperature ranges on small spatial scales and short timescales, making them difficult to observe with current instrumentation. The upcoming SOLAR-C mission, launching in the late 2020s, will provide unprecedented plasma diagnostic capability with its high-throughput extreme-ultraviolet (EUV) spectroscopic telescope (EUVST), capable of ~0.2 arcsec/pix spatial sampling (~0.4 arcsec resolution), continuous temperature coverage from 0.02-15 MK, and exposure times down to 0.5 seconds. We present forward modelling of the spectrograph's short wavelength camera (170-210 Å; SOLAR-C/EUVST-SW) and its response to log T~6.2 coronal plasma in a three-dimensional MHD-simulated pre-flare active region. We compare this performance to that of the previous-generation EUV Imaging Spectrometer (EIS) on Hinode (SOLAR-B). Our results demonstrate that SOLAR-C/EUVST can distinguish individual flux tubes in simulated active region loops which Hinode/EIS cannot resolve. In simulated pre-flare plasma, SOLAR-C/EUVST captures sharp velocity gradients between adjacent upflowing and downflowing plasma which Hinode/EIS is unable to resolve. Doppler velocity measurement accuracy will reach better than 1 km/s in active regions. We show that this next-generation spectrograph can be expected to directly observe processes potentially related to flare triggering, such as plasma flows from low-altitude reconnection linked to emerging flux, and determine whether active region loops consist of a small number of strands or the hundreds predicted by magnetic reconnection-induced nanoflare heating models.
