NUMERICAL SIMULATIONS OF CORONAL MASS EJECTION ON 2011 MARCH 7: ONE-TEMPERATURE AND TWO-TEMPERATURE MODEL COMPARISON
NUMERICAL SIMULATIONS OF CORONAL MASS EJECTION ON 2011 MARCH 7: ONE-TEMPERATURE AND TWO-TEMPERATURE MODEL COMPARISON
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DOI：
10.1088/0004-637x/773/1/50
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发表时间：
2013-07
期刊：
影响因子：
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通讯作者：
M. Jin;W. Manchester;B. van der Holst;R. Oran;I. Sokolov;G. Tóth;Y. Liu;X. Sun;T. Gombosi
中科院分区：
文献类型：
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作者：
M. Jin;W. Manchester;B. van der Holst;R. Oran;I. Sokolov;G. Tóth;Y. Liu;X. Sun;T. Gombosi
在卡林顿自转（CR）2107年期间，活动区NOAA 11164发生了一次快速日冕物质抛射（CME; >2000 km s−1）。这一事件也与太阳高能粒子事件有关。在这项研究中，我们提出了一个温度（1 T）和两个温度（2 T：电子和质子的人口耦合热力学）模型的模拟。1 T和2 T模型都是从色球层开始的，具有热传导和辐射冷却。背景太阳风由阿尔文波压力驱动，并由阿尔文波耗散加热，其中我们在闭合场线顶部加入了平衡湍流。内边界的磁场是使用太阳动力学观测台/日震和磁成像仪的天气图建立的。Titov-Démoulin磁通绳模型被用来启动CME事件。我们比较了1 T和2 T CME模拟中快速CME的传播和CME驱动冲击的热力学。此外，合成的白色光图像与太阳和日光层天文台/大角度和光谱日冕观测进行了比较。由于电子和质子温度之间没有区别，1 T模型中的热传导在CME驱动的冲击之前产生了非物理的温度前兆，并使冲击参数（例如，激波马赫数、压缩比）不正确。我们的研究结果表明，电子热传导与质子冲击加热，以产生物理上正确的CME结构和CME驱动的冲击的重要性。
During Carrington rotation (CR) 2107, a fast coronal mass ejection (CME; >2000 km s−1) occurred in active region NOAA 11164. This event is also associated with a solar energetic particle event. In this study, we present simulations of this CME with one-temperature (1T) and two-temperature (2T: coupled thermodynamics of the electron and proton populations) models. Both the 1T and 2T models start from the chromosphere with heat conduction and radiative cooling. The background solar wind is driven by Alfvén-wave pressure and heated by Alfvén-wave dissipation in which we have incorporated the balanced turbulence at the top of the closed field lines. The magnetic field of the inner boundary is set up using a synoptic map from Solar Dynamics Observatory/Helioseismic and Magnetic Imager. The Titov–Démoulin flux-rope model is used to initiate the CME event. We compare the propagation of fast CMEs and the thermodynamics of CME-driven shocks in both the 1T and 2T CME simulations. Also, the synthesized white light images are compared with the Solar and Heliospheric Observatory/Large Angle and Spectrometric Coronagraph observations. Because there is no distinction between electron and proton temperatures, heat conduction in the 1T model creates an unphysical temperature precursor in front of the CME-driven shock and makes the shock parameters (e.g., shock Mach number, compression ratio) incorrect. Our results demonstrate the importance of the electron heat conduction in conjunction with proton shock heating in order to produce the physically correct CME structures and CME-driven shocks.