SIMULTANEOUS IRIS AND HINODE/EIS OBSERVATIONS AND MODELING OF THE 2014 OCTOBER 27 X2.0 CLASS FLARE
SIMULTANEOUS IRIS AND HINODE/EIS OBSERVATIONS AND MODELING OF THE 2014 OCTOBER 27 X2.0 CLASS FLARE
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DOI：
10.3847/0004-637x/816/2/89
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发表时间：
2015-12
期刊：
影响因子：
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通讯作者：
V. Polito;J. Reep;J. Reep;K. Reeves;P. Simões;J. Dudík;G. Zanna;H. Mason;L. Golub
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文献类型：
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作者：
V. Polito;J. Reep;J. Reep;K. Reeves;P. Simões;J. Dudík;G. Zanna;H. Mason;L. Golub
我们对2014年10月27日发生的X2级耀斑进行了研究，并用Hinode卫星上的界面区域成像光谱仪（IRIS）和EUV成像光谱仪（EIS）进行了观测。由于IRIS和EIS仪器的高节奏和空间分辨率，我们能够比较色球蒸发阶段耀斑带中Fe xxi 1354.08 Å和Fe xxiii 263.77 Å高温发射（10 MK）的同时观测结果。我们发现IRIS观测到完全蓝移的Fe xxi谱线，在耀斑的上升阶段高达200 km s − 1，表明等离子体上升流的位置被IRIS分辨。相比之下，Fe XXIII线通常是不对称的，我们将其解释为由于EIS的空间分辨率较低。SDO/AIA和Hinode/XRT的温度估计表明，热发射（log（T [K]）> 7.2）首先集中在足点，然后填充环。来自IRIS和EIS的密度敏感谱线估计，在脉冲阶段，过渡区谱线的电子数密度为1012 cm − 3，日冕谱线的电子数密度为1010 cm − 3。为了将观测结果与理论预测进行比较，我们使用HYDRAD 1D Hydro代码对正在加热的耀斑环进行了模拟。我们发现，模拟的等离子体参数是接近的观测值，得到与IRIS，Hinode，和AIA。这些结果支持电子束加热模型，而不是一个纯粹的热传导模型作为驱动机制，这个耀斑。
We present a study of the X2-class flare which occurred on 2014 October 27 and was observed with the Interface Region Imaging Spectrograph (IRIS) and the EUV Imaging Spectrometer (EIS) on board the Hinode satellite. Thanks to the high cadence and spatial resolution of the IRIS and EIS instruments, we are able to compare simultaneous observations of the Fe xxi 1354.08 Å and Fe xxiii 263.77 Å high-temperature emission (≳10 MK) in the flare ribbon during the chromospheric evaporation phase. We find that IRIS observes completely blueshifted Fe xxi line profiles, up to 200 km s−1 during the rise phase of the flare, indicating that the site of the plasma upflows is resolved by IRIS. In contrast, the Fe xxiii line is often asymmetric, which we interpret as being due to the lower spatial resolution of EIS. Temperature estimates from SDO/AIA and Hinode/XRT show that hot emission (log(T[K]) > 7.2) is first concentrated at the footpoints before filling the loops. Density-sensitive lines from IRIS and EIS give estimates of electron number density of ≳1012 cm−3 in the transition region lines and 1010 cm−3 in the coronal lines during the impulsive phase. In order to compare the observational results against theoretical predictions, we have run a simulation of a flare loop undergoing heating using the HYDRAD 1D hydro code. We find that the simulated plasma parameters are close to the observed values that are obtained with IRIS, Hinode, and AIA. These results support an electron beam heating model rather than a purely thermal conduction model as the driving mechanism for this flare.