The Origin of Solar Filament Plasma Inferred from In Situ Observations of Elemental Abundances
The Origin of Solar Filament Plasma Inferred from In Situ Observations of Elemental Abundances
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从元素丰度的原位观测推断太阳丝等离子体的起源
DOI：
10.3847/2041-8213/aa5d54
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发表时间：
2017-02
期刊：
影响因子：
--
通讯作者：
Zhang J.
中科院分区：
文献类型：
--
作者：
Song H. Q.;Chen Y.;Li B.;Li L. P.;Zhao L.;He J. S.;Duan D.;Cheng X.;Zhang J.
太阳暗条/日冕是日冕中最常见的特征之一，当它们爆发时，可能会导致高能日冕物质抛射（CME）和耀斑。灯丝的温度和密度是日冕物质的100倍，对它们的物质来源的物理理解仍然存在争议。有两种假设：一种认为丝状等离子体是通过虹吸或蒸发/注入过程从光球层或色球层进入日冕的，另一种认为是由于热不稳定性，物质从周围的日冕等离子体中凝结而成。元素丰度分析是一个合理的线索，以约束模型，虹吸或蒸发/注入模型将预测灯丝材料的丰度接近光球或色球的，而冷凝模型应该有日冕的丰度。在这封信中，我们分析了包含喷出的细丝材料的磁云的元素丰度。对应的暗条爆发发生在1998年4月29日，伴随着位于日面坐标S18 E20（NOAA 08210）的M6.8级软X射线耀斑和太阳附近线速度为1374 km s−1的快晕CME。结果表明，第一电离势低和高的元素Fe/O、Mg/O和Si/O的丰度比分别为0.150、0.050和0.070，接近它们对应的光球值0.065、0.081和0.066，这不支持丝状等离子体的日冕起源。
Solar filaments/prominences are one of the most common features in the corona, which may lead to energetic coronal mass ejections (CMEs) and flares when they erupt. Filaments are about 100 times cooler and denser than the coronal material, and physical understanding of their material origin remains controversial. Two types of scenarios have been proposed: one argues that the filament plasma is brought into the corona from photosphere or chromosphere through a siphon or evaporation/injection process, while the other suggests that the material condenses from the surrounding coronal plasma due to thermal instability. The elemental abundance analysis is a reasonable clue to constrain the models, as the siphon or evaporation/injection model would predict that the filament material abundances are close to the photospheric or chromospheric ones, while the condensation model should have coronal abundances. In this Letter, we analyze the elemental abundances of a magnetic cloud that contains the ejected filament material. The corresponding filament eruption occurred on 1998 April 29, accompanying an M6.8 class soft X-ray flare located at the heliographic coordinates S18E20 (NOAA 08210) and a fast halo CME with the linear velocity of 1374 km s−1 near the Sun. We find that the abundance ratios of elements with low and high first ionization potential such as Fe/O, Mg/O, and Si/O are 0.150, 0.050, and 0.070, respectively, approaching their corresponding photospheric values 0.065, 0.081, and 0.066, which does not support the coronal origin of the filament plasma.
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作者：
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发表时间：
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