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首页> 外文期刊>PASJ: Publications of the Astronomical Society of Japan >Blue-wing enhancement of the chromospheric Mg II h and k lines in a solar flare
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Blue-wing enhancement of the chromospheric Mg II h and k lines in a solar flare

机译：太阳耀斑的致铬选手Mg II H和K线的蓝翼增强

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We performed coordinated observations of AR 12205, which showed a C-class flare on 2014 November 11, with the Interface Region Imaging Spectrograph (IRIS) and the Domeless Solar Telescope (DST) at Hida Observatory. Using spectral data in the Si IV 1403 angstrom, Cu II 1335 angstrom, and Mg II h and k lines from IRIS and the Ca II K, Ca II 8542 angstrom, and H alpha lines from DST, we investigated a moving flare kernel during the flare. In the Mg II h line, the leading edge of the flare kernel showed an intensity enhancement in the blue wing and a smaller intensity of the blue-side peak (h2v) than that of the red-side one (h2r). The blueshift lasted for 9-48 s with a typical speed of 10.1 +/- 2.6 km s(-1), which was followed by a high intensity and a large redshift with a speed of up to 51 km s(-1) detected in the Mg II h line. The large redshift was a common property for all six lines, but the blueshift prior to it was found only in the Mg II lines. Cloud modeling of the Mg II h line suggests that the blue-wing enhancement with such a peak difference could have been caused a chromospheric-temperature (cool) upflow. We discuss a scenario in which an upflow of cool plasma is lifted up by expanding hot plasma owing to the deep penetration non-thermal electrons into the chromosphere. Furthermore, we found that the blueshift persisted without any subsequent redshift in the leading edge of the flare kernel during its decaying phase. The cause of such a long-lasting blueshift is also discussed.
机译：我们对AR 12205进行了协调观察，该协调了2014年11月11日的C级耀斑，界面区域成像光谱仪（IRIS）和HIDA天文台的无国内太阳能望远镜（DST）。使用Si IV 1403 Angstrom中的光谱数据，Cu II 1335 Angstrom和来自IRIS的Ca II k，Ca II 8542埃与DST的Ca II K，Ca II 8542埃α和Hα线，我们调查了一个移动的火炬内核耀斑。在Mg II H线中，闪光核的前缘显示出蓝翼的强度增强和比红色侧（H2R）的蓝侧峰（H2V）的较小强度。 BlueShift持续了9-48秒，典型速度为10.1 +/- 2.6 km s（-1），然后是高强度和大型红移，速度可达51 km s（-1）在Mg II H线。大型红移是所有六条线的常见物业，但在它之前的平淡无奇于Mg II线。 Mg II H线的云建模表明，具有这种峰值差异的蓝翼增强可能已经引起了溢出的​​溢出量（酷）溢出。我们讨论了一种情况，其中通过将热等离子体扩展到铬层的深渗透性，通过膨胀热等离子体来提升冷等离子体的上流。此外，我们发现蓝色在衰变阶段期间没有在闪光内核的前缘中的任何后续射频的情况下坚持不懈。还讨论了这种长期蓝色的原因。

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