One of the key processes associated with the “standard” flare model is chromospheric evaporation, a process during which plasma heated to high temperatures by energy deposition at the flare footpoints is driven upwards into the corona. Despite several decades of study, a number of open questions remain, including the relationship between plasma produced during this process and observations of earlier “superhot” plasma. The Extreme ultraviolet Imaging Spectrometer (EIS) onboard Hinode has a wide slot, which is often used as a flare trigger in the He ii emission-line band. Once the intensity passes a threshold level, the study will switch to one focussed on the flaring region. However, when the intensity is not high enough to reach the flare trigger threshold, these datasets are then available during the entire flare period and provide high-cadence spectroscopic observations over a large field of view. We make use of data from two such studies of a C4.7 flare and a C1.6 flare to probe the relationship between hot Fe xxiv plasma and plasmas observed by the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) and the X-ray Telescope (XRT) to track where the emission comes from and when it begins. The flare trigger slot data used in our analysis has one-minute cadence. Although the spatial and spectral information are merged in the wide-slot data, it is still possible to extract when the hot plasma appears, through the appearance of the Fe x xiv spectral image. It is also possible to derive spectrally pure Fe xxiv light curves from the EIS data, and compare them with those derived from hard X-rays, enabling a full exploration of the evolution of hot emission. The Fe xxiv emission peaks just after the peak in the hard X-ray lightcurve; consistent with an origin in the evaporation of heated plasma following the transfer of energy to the lower atmosphere. A peak was also found for the C4.7 flare in the RHESSI peak temperature, which occurred before the hard X-rays peaked. This suggests that the first peak in hot-plasma emission is likely to be directly related to the energy-release process.

中文翻译：

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使用来自 Hinode EUV 成像光谱仪的光谱重叠图数据定位小耀斑中的热等离子体

与“标准”耀斑模型相关的关键过程之一是色球蒸发，在此过程中，通过耀斑足点处的能量沉积加热到高温的等离子体被向上驱动到日冕中。尽管进行了几十年的研究，但仍有许多悬而未决的问题，包括在此过程中产生的等离子体与早期“超热”等离子体的观察结果之间的关系。Hinode 上的极紫外成像光谱仪 (EIS) 有一个宽槽，通常用作 He ii 发射线波段的耀斑触发器。一旦强度超过阈值水平，研究将切换到专注于耀斑区域的研究。但是，当强度不足以达到耀斑触发阈值时，然后，这些数据集在整个耀斑期间都可用，并提供大视野内的高节奏光谱观测。我们利用来自 C4.7 耀斑和 C1.6 耀斑的两项此类研究的数据来探讨热 Fe xxiv 等离子体与 Reuven Ramaty 高能太阳光谱成像仪 (RHESSI) 和 X 射线观测到的等离子体之间的关系望远镜 (XRT) 来跟踪发射的来源和开始时间。我们分析中使用的耀斑触发槽数据具有一分钟的节奏。虽然空间和光谱信息融合在宽槽数据中，但仍然可以通过 Fe x xiv 光谱图像的出现来提取热等离子体何时出现。也可以从 EIS 数据导出光谱纯 Fe xxiv 光曲线，并将它们与来自硬 X 射线的那些进行比较，从而能够全面探索热发射的演变。Fe xxiv 发射峰紧接在硬 X 射线光曲线峰之后；与能量转移到低层大气后加热等离子体蒸发的起源一致。在 RHESSI 峰值温度中也发现了 C4.7 耀斑的峰值，它发生在硬 X 射线达到峰值之前。这表明热等离子体发射的第一个峰值可能与能量释放过程直接相关。RHESSI 峰值温度出现 7 次耀斑，发生在硬 X 射线达到峰值之前。这表明热等离子体发射的第一个峰值可能与能量释放过程直接相关。RHESSI 峰值温度出现 7 次耀斑，发生在硬 X 射线达到峰值之前。这表明热等离子体发射的第一个峰值可能与能量释放过程直接相关。