典型太阳耀斑的多波长观测和模拟
Multi-wavelength observations and modelling of a canonical solar flare
摘要：
本文从观测和理论两个方面研究了C级太阳耀斑中温度、辐射量、能量损失和速度的时间演化。耀斑的性质是通过RHESSI（>5 MK）、GOES-12（5-30 MK）、TRACE 171 A（1 MK）和SOHO/CDS（~0.03-8 MK）等仪器的响应函数跟踪等离子体的系统冷却而得出的。这些测量结合从0-D EBTEL模型的模拟进行了研究。在耀斑爆发时，在Fe XIX中观察到~90 km s-1的上升流和低水平发射，与耀斑前加热和温和的色球蒸发一致。在脉冲阶段，上升流的~80公里s-1的Fe XIX和同时下降流的20公里s-1的He I和O V，表明爆炸性色球蒸发。随后发现血浆在约10分钟内达到约13 MK的峰值温度。使用EBTEL，传导被发现是主要的损耗机制在衰减阶段的初始~ 300 s。它也被发现是负责驱动温和的色球蒸发在此期间。随着温度下降到约8 MK以下，并且在接下来的约4,000 s内，辐射损耗被确定为主导传导损耗。辐射损失阶段是伴随着显着的下降流<40公里s-1的O V。这是第一次广泛的研究的一个典型的太阳耀斑的演变使用光谱和宽带仪器结合流体动力学模型。虽然我们的研究结果与标准耀斑模型基本一致，但模拟结果表明，至少在此事件的脉冲阶段，传导和非热束加热在加热耀斑等离子体中起着重要作用。
英文摘要：
This paper investigates the temporal evolution of temperature, emission measure, energy loss and velocity in a C-class solar flare from both an observational and theoretical perspective. The properties of the flare were derived by following the systematic cooling of the plasma through the response functions of a number of instruments -- RHESSI (>5 MK), GOES-12 (5-30 MK), TRACE 171 A (1 MK) and SOHO/CDS (~0.03-8 MK). These measurements were studied in combination with simulations from the 0-D EBTEL model. At the flare on-set, upflows of ~90 km s-1 and low level emission were observed in Fe XIX, consistent with pre-flare heating and gentle chromospheric evaporation. During the impulsive phase, upflows of ~80 km s-1 in Fe XIX and simultaneous downflows of 20 km s-1 in He I and O V were observed, indicating explosive chromospheric evaporation. The plasma was subsequently found to reach a peak temperature of ~13 MK in approximately 10 minutes. Using EBTEL, conduction was found to be the dominant loss mechanism during the initial ~300s of the decay phase. It was also found to be responsible for driving gentle chromospheric evaporation during this period. As the temperature fell below ~8 MK, and for the next ~4,000s, radiative losses were determined to dominate over conductive losses. The radiative loss phase was accompanied by significant downflows of <40 km s-1 in O V. This is the first extensive study of the evolution of a canonical solar flare using both spectroscopic and broad-band instruments in conjunction with a hydrodynamic model. While our results are in broad agreement with the standard flare model, the simulations suggest that both conductive and non-thermal beam heating play important roles in heating the flare plasma during the impulsive phase of at least this event.
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