We report multi-wavelength observations of four solar flares on 2014 July 07. We firstly select these flares according to the soft X-ray (SXR) and extreme ultraviolet (EUV) emissions recorded by the Extreme Ultraviolet Variability Experiment and Geostationary Orbiting Environmental Satellites. Then their locations and geometries are identified from the full-disk images measured by the Atmospheric Imaging Assembly (AIA), and the time delays among the light curves in different channels are identified. The electron number densities are estimated using the differential emission measure method. We find that three of four flares show strong emissions in SXR channels and high temperature (>6 MK) EUV wavelengths during the impulsive phase, i.e., AIA 131 and 94 , and then they emit peak radiation subsequently in the middle temperature (∼0.6−3 MK) EUV channels. Moreover, they last for a long time and have smaller electron densities, which are probably driven by the interaction of hot diffuse flare loops. Only one flare emits radiation at almost the same time in all the observed wavelengths, lasts for a relatively short time, and has a larger electron density. It is also accompanied by a type III radio burst. The bright emission at the EUV channel could be corresponding to the associated erupting filament.

我们于 2014 年 7 月 7 日报告了对四个太阳耀斑的多波长观测。我们首先根据极紫外变异实验和地球静止轨道环境卫星记录的软 X 射线（SXR）和极紫外（EUV）发射选择这些耀斑。然后从大气成像组件（AIA）测量的全盘图像中识别它们的位置和几何形状，并识别不同通道中光曲线之间的时间延迟。使用差分发射测量方法估计电子数密度。我们发现四个耀斑中有三个在脉冲阶段在 SXR 通道和高温（>6 MK） EUV 波长中显示出强烈的发射，即 AIA 131 和 94，然后它们随后在中间温度（~0. 6−3 MK) EUV 通道。此外，它们持续时间长且电子密度较小，这可能是由热漫射耀斑环的相互作用驱动的。在所有观察到的波长中，只有一个耀斑几乎同时发射辐射，持续时间相对较短，并且具有较大的电子密度。它还伴随着 III 型射电暴。EUV 通道上的明亮发射可能对应于相关的喷发灯丝。