论文标题
通话和反应：大太阳耀斑中色球蒸发的时间分辨研究
Call and Response: A Time-Resolved Study of Chromospheric Evaporation in a Large Solar Flare
论文作者
论文摘要
我们研究了NOAA AR 12602在2014年10月22日生产的X1.6太阳耀斑。此事件的整个耀斑均由Rhessi，Iris和Hinode/eis涵盖，从而允许分析对非热电子驱动器的色球反应。我们通过Rhessi光谱拟合得出了非热电子中包含的能量，并将此调用的时间依赖性参数与跨温度范围内多普勒速度，密度和非热宽度的响应联系起来。注入的总能量为$ 4.8 \ times10^{30} $ erg，持续$ 352 $秒。这种能量驱动了爆炸性的色球蒸发，在流动逆转温度（1.35--1.82 mk之间）的多普勒和非热速度的描述。峰值电子注射时间（14:06 UT）对应于最高速度的时间。目前，我们在Fe XXIV的核心中发现了200 km s $^{ - 1} $ blueshifts，通常假定这是静止的。在此之前不久，非热电子总体具有最浅的光谱指数（$ \ $ 6），对应于Si IV和Fe XXI中的峰值非热速度。 Fe XIV中的非热速度在流动逆转温度附近形成的速度较低，与密度或多普勒速度无关。观察到温度相似的离子中的非热速度与多普勒速度增加并相关，这意味着周围的流动逆转点尚未解决。这项研究为大型X级耀斑提供了一组全面的，时间分辨的色球诊断，以及时间分辨的能量注入曲线，非常适合进一步建模研究。
We studied an X1.6 solar flare produced by NOAA AR 12602 on 2014 October 22. The entirety of this event was covered by RHESSI, IRIS, and Hinode/EIS, allowing analysis of the chromospheric response to a nonthermal electron driver. We derived the energy contained in nonthermal electrons via RHESSI spectral fitting, and linked the time-dependent parameters of this call to the response in Doppler velocity, density, and nonthermal width across a broad temperature range. The total energy injected was $4.8\times10^{30}$ erg, and lasted $352$ seconds. This energy drove explosive chromospheric evaporation, with a delineation in both Doppler and nonthermal velocities at the flow reversal temperature, between 1.35--1.82 MK. The time of peak electron injection (14:06 UT) corresponded to the time of highest velocities. At this time, we found 200 km s$^{-1}$ blueshifts in the core of Fe XXIV, which is typically assumed to be at rest. Shortly before this time, the nonthermal electron population had the shallowest spectral index ($\approx$ 6), corresponding to the peak nonthermal velocity in Si IV and Fe XXI. Nonthermal velocities in Fe XIV, formed near the flow reversal temperature were low, and not correlated with density or Doppler velocity. Nonthermal velocities in ions with similar temperatures were observed to increase and correlate with Doppler velocities, implying unresolved flows surrounding the flow reversal point. This study provides a comprehensive, time-resolved set of chromospheric diagnostics for a large X-class flare, along with a time-resolved energy injection profile, ideal for further modeling studies.
