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首页> 外文期刊>The Astrophysical journal >RECONCILING HYDRODYNAMIC SIMULATIONS WITH SPECTROSCOPIC OBSERVATIONS OF SOLAR FLARES
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RECONCILING HYDRODYNAMIC SIMULATIONS WITH SPECTROSCOPIC OBSERVATIONS OF SOLAR FLARES

机译：水动力模拟与太阳耀斑光谱观测的协调

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摘要

Chromospheric evaporation is a central element of current models of solar flares. The high-velocity upflows that should accompany evaporation, however, are rarely observed in high-resolution solar flare spectra. Thus the absence of blueshifted line profiles represents a significant discrepancy between the theory and observations of this phenomenon. In this Letter we present an algorithm for computing multiple-loop time-dependent hydrody-namic simulations of solar flares using a minimum of assumptions. We show that these simulations can accurately reproduce the Ca XIX and S XV line profiles observed with the Bragg Crystal Spectrometer on Yohkoh during the earliest stages of a flare. Since our model represents the flare as a succession of independently heated threads, the strongly blueshifted emission evident during the initial heating of a thread is largely masked by emission from threads that have been heated previously and do not show bulk motions.
机译：大气层蒸发是当前太阳耀斑模型的核心要素。然而，在高分辨率的太阳耀斑光谱中很少观察到伴随蒸发的高速上升流。因此，没有蓝移线轮廓表示该现象的理论与观察结果之间存在重大差异。在这封信中，我们提出了一种使用最少的假设来计算太阳耀斑的多回路时间相关的水动力模拟的算法。我们表明，这些模拟可以准确地再现在火炬最早阶段用Yohkoh上的Bragg晶体光谱仪观测到的Ca XIX和S XV线轮廓。由于我们的模型将火炬表示为一连串独立加热的线，因此，在线的初始加热过程中出现的强烈蓝移的发射在很大程度上被先前已加热且不显示整体运动的线的发射所掩盖。

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