SIMULATIONS OF THE MG ii K AND CA ii 8542 LINES FROM AN ALFVÉN WAVE-HEATED FLARE CHROMOSPHERE
SIMULATIONS OF THE MG ii K AND CA ii 8542 LINES FROM AN ALFVÉN WAVE-HEATED FLARE CHROMOSPHERE
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DOI：
10.3847/0004-637x/827/2/101
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发表时间：
2016-05
期刊：
影响因子：
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通讯作者：
G. Kerr;L. Fletcher;A. Russell;J. Allred
中科院分区：
文献类型：
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作者：
G. Kerr;L. Fletcher;A. Russell;J. Allred
我们使用辐射流体动力学模拟研究太阳耀斑色球加热的两种模型：阿尔文波耗散和电子束碰撞损失。这两种机制都能够强大的色球加热，我们表明，独特的大气演变中上部色球的结果在镁二K线发射波加热和光束加热模拟之间应该是明显不同的。我们还展示了在色球层稍深处形成的Ca ii 8542 Å轮廓。从我们的波加热模拟的Mg II的k-线的配置文件是完全不同的，从光束加热模型，更符合界面区域成像光谱仪观测。两个模型中Ca ii 8542的预测差异很小。我们的结论是，仔细的观测和理论研究中上部色球层形成的线具有真正的承诺，区分色球加热耀斑的竞争模型。
We use radiation hydrodynamic simulations to examine two models of solar flare chromospheric heating: Alfvén wave dissipation and electron beam collisional losses. Both mechanisms are capable of strong chromospheric heating, and we show that the distinctive atmospheric evolution in the mid-to-upper chromosphere results in Mg ii k-line emission that should be observably different between wave-heated and beam-heated simulations. We also present Ca ii 8542 Å profiles that are formed slightly deeper in the chromosphere. The Mg ii k-line profiles from our wave-heated simulation are quite different from those from a beam-heated model and are more consistent with Interface Region Imaging Spectrograph observations. The predicted differences between the Ca ii 8542 Å in the two models are small. We conclude that careful observational and theoretical study of lines formed in the mid-to-upper chromosphere holds genuine promise for distinguishing between competing models for chromospheric heating in flares.