H a AND EUV OBSERVATIONS OF A PARTIAL CME
H a AND EUV OBSERVATIONS OF A PARTIAL CME
复制标题
部分 CME 的 H a 和 EUV 观测
DOI：
10.1088/0004-637x/804/2/147
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发表时间：
2015
期刊：
影响因子：
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通讯作者：
Christian D
中科院分区：
文献类型：
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作者：
Christian D
我们已经获得了上层太阳色球层的Hα高空间和时间分辨率观测结果，并通过太阳动力学天文台（SDO）和日出极紫外成像光谱仪的多波长观测结果对这些观测结果进行了补充。 Hα 观测是在 2012 年 2 月 11 日使用国家太阳天文台邓恩太阳望远镜的氢-阿尔法快速动力学相机仪器进行的。我们的 Hα 观测发现，日珥喷发失败后，有大量色球物质从日冕高度返回。我们在 Hα 和几个 SDO 大气成像组件带通中检测到几个大型凝结（“斑点”）以 200 km s−1 的速度返回太阳表面。 Hα中这些“斑点”的平均导出尺寸在垂直于行进方向和平行于行进方向的方向上分别为500×3000km 2 。将我们的“斑点”宽度与日冕雨中发现的“斑点”宽度进行比较，表明存在额外的、更小的、未解决的“斑点”，这与之前的研究和最近的数值模拟一致。我们在 Hα 和 SDO 波段中观察到的“斑点”的速度和减速度小于重力自由落体的预期速度和减速度，这意味着额外的磁力或气压阻碍了流动。我们推导出主喷发的动能比典型的日冕物质抛射低约 2 个数量级，这可以解释其部分性质。
We have obtained Hα high spatial and time resolution observations of the upper solar chromosphere and supplemented these with multi-wavelength observations from the Solar Dynamics Observatory (SDO) and the Hinode Extreme-ultraviolet Imaging Spectrometer. The Hα observations were conducted on 2012 February 11 with the Hydrogen-Alpha Rapid Dynamics Camera instrument at the National Solar Observatory's Dunn Solar Telescope. Our Hα observations found large downflows of chromospheric material returning from coronal heights following a failed prominence eruption. We have detected several large condensations (" blobs") returning to the solar surface at velocities of≈ 200 km s− 1 in both Hα and several SDO Atmospheric Imaging Assembly band passes. The average derived size of these" blobs" in Hα is 500 by 3000 km 2 in the directions perpendicular and parallel to the direction of travel, respectively. A comparison of our" blob" widths to those found from coronal rain, indicate that there are additional, smaller, unresolved" blobs" in agreement with previous studies and recent numerical simulations. Our observed velocities and decelerations of the" blobs" in both Hα and SDO bands are less than those expected for gravitational free-fall and imply additional magnetic or gas pressure impeding the flow. We derived a kinetic energy of≈ 2 orders of magnitude lower for the main eruption than a typical coronal mass ejection, which may explain its partial nature.