The 1991 November 9 flare at 03.2 UT: Observations from Yohkoh
The 1991 November 9 flare at 03.2 UT: Observations from Yohkoh
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1991 年 11 月 9 日 03.2 UT 耀斑：来自 Yohkoh 的观测
DOI：
10.1086/174540
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发表时间：
1994
期刊：
影响因子：
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通讯作者：
Tetsuya Watanabe
中科院分区：
文献类型：
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作者：
G. Doschek;J. Mariska;K. Strong;R. Bentley;C. Brown;J. Culhane;J. Lang;A. Sterling;Tetsuya Watanabe
我们讨论了1991年11月9日发生在03.2 UT附近的M1.9耀斑的X射线谱和软X射线图像。这些数据是用日本Yohkoh航天器上的仪器获得的。它们涵盖了整个上升阶段和峰值耀斑发射，以及衰减阶段的开始。我们确定的动力学，温度和排放量的耀斑推断从X射线谱线的Fe XXV，Ca XIX，和S XV的共振线。我们讨论了从软X射线图像推断的耀斑形态。11月9日的耀斑是非典型的，因为在耀斑爆发时，共振线观察到比通常更强的蓝移发射分量（相对于静止分量）。我们讨论了几种方法去卷积的蓝移分量从固定的组成部分。的X射线线轮廓是一致的色球蒸发的数值模拟的预测。X射线图像揭示了一个复杂的环几何形状的耀斑，这是不完全理解。图像中的许多特征都在以几公里/秒到大约800公里/秒的速度向上移动。蓝移的发射开始于硬X射线发射的开始附近，这意味着粒子加速和上升的等离子体具有共同的能量源。
We discuss X-ray spectra and soft X-ray images of an M1.9 flare that occurred on 1991 November 9 near 03.2 UT. These data were obtained with instrumentation on the Japanese Yohkoh spacecraft. They cover the entire rise phase and peak flare emission, and the beginning of the decay phase. We determine the dynamics, temperature, and emission measure of the flare as inferred from the X-ray line profiles of resonance lines of Fe XXV, Ca XIX, and S XV. We discuss the morphology of the flare as inferred from the soft X-ray images. The November 9 flare is atypical in that a stronger than usual blueshifted emission component (relative to the stationary component) is observed for the resonance lines at flare onset. We discuss several methods for deconvolving the blueshifted component from the stationary component. The X-ray line profiles are consistent with predictions of numerical simulations of chromospheric evaporation. The X-ray images reveal a flare with a complicated loop geometry that is not fully understood. Many of the features in the images are moving upwards at speeds ranging from a few km/s to about 800 km/s. The blueshifted emission begins near the onset of hard X-ray emission, implying that particle acceleration and upflowing plasma have a common energy source.