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The White-Light Limb Flare of 16 August 1989 and its Chromospheric Counterpart

机译:1989年8月16日的白光肢体耀斑及其色温对应

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摘要

After carefully comparing the white-light (5600±00 Å) and the slit-jaw Hα images (0.5 Å passband) of the 2N/X20 white-light flare of 16 August 1989, we found that the Hα counterpart identification of the bright kernels in continuum by Hiei, Nakagomi, and Takuma (1992) was incorrect. Now we come to the conclusion that none of the two white-light kernels has a corresponding bright Hα area. Moreover, the loop shapes in white-light are also different from those in Hα. Hα loops rose more rapidly than white-light loops. However, their height–time variations on the whole are similar. This indicates that the continuum and chromospheric emissions of the flare presumably come from different plasmas, but may be modulated by some mutual factors, such as large-scale magnetic fields. Analysis of the He i 10 830 Å spectra taken simultaneously with the slit-jaw Hα images shows that the line-center intensity of He i 10 830 Å doesn't have a good correlation with the intensity of nearby continuum, which supports the above conclusions. In addition, the electron density at the white-light loop top estimated from the continuum around 5600 Å and 10 830 Å is as high as 1012–1013 cm−3.
机译:在仔细比较了1989年8月16日的2N / X20白光耀斑的白光(5600±00Å)和狭缝下颌Hα图像(通带0.5Å)后,我们发现了明亮核仁的Hα对应物鉴定Hiei,Nakagomi和Takuma(1992)提出的连续论是错误的。现在我们得出的结论是,两个白光内核都没有相应的明亮Hα区域。而且,白光下的回路形状也与Hα不同。 Hα环比白光环上升得更快。但是,它们的高度-时间变化总体上是相似的。这表明火炬的连续性和色球发射可能来自不同的等离子体,但是可能受到某些互为因素的调制,例如大范围的磁场。与狭缝下颌Hα图像同时拍摄的He i 10 830Å光谱的分析表明,He i 10 830Å的线心强度与附近连续谱的强度没有很好的相关性,这支持上述结论。 。此外,从5600Å和10 830Å附近的连续峰估计的白光回路顶部的电子密度高达1012 –1013 cm-3

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  • 来源
    《Solar Physics》 |2003年第2期|235-245|共11页
  • 作者

    Jianqi You; Eijiro Hiei; Hui Li;

  • 作者单位

    Purple Mountain Observatory Chinese Academy of Sciences;

    National Astronomical Observatory of Japan Mitaka;

    Purple Mountain Observatory Chinese Academy of Sciences;

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  • 正文语种 eng
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