X-rays and extreme ultraviolet (EUV) emissions from solar flares rapidly change the physical composition of the Earth’s thermosphere and ionosphere, thereby causing space weather phenomena such as communication failures. Numerous empirical and physical models have been developed to estimate the effects of flare emissions on the Earth’s upper atmosphere. We verified the reproduction of the flare emission spectra using a one-dimensional hydrodynamic calculation and the CHIANTI atomic database. To validate the proposed model, we used the observed EUV spectra obtained by the Extreme ultraviolet variability experiment (EVE) on board the Solar Dynamics Observatory (SDO). We examined the “EUV flare time-integrated irradiance” and “EUV flare line rise time” of the EUV emissions for 21 events by comparing the calculation results of the proposed model and observed EUV spectral data. The proposed model successfully reproduced the EUV flare time-integrated irradiance of the Fe VIII 131 Å, Fe XVIII 94 Å, and Fe XX133 Å, as well as the 55–355 Å and 55–135 Å bands. For the EUV flare line rise time, there was an acceptable correlation between the proposed model estimations and observations for all Fe flare emission lines. These results demonstrate that the proposed model can reproduce the EUV flare emission spectra from the emitting plasma with a relatively high formation temperature. This indicates that the physics-based model is effective for the accurate reproduction of the EUV spectral irradiance.

太阳耀斑产生的X射线和极紫外（EUV）辐射迅速改变了地球热层和电离层的物理组成，从而导致了空间天气现象，例如通信故障。已经开发了许多经验和物理模型来估计火炬排放对地球高层大气的影响。我们使用一维水动力计算和CHIANTI原子数据库验证了火炬发射光谱的再现。为了验证所提出的模型，我们使用了由太阳动力学天文台（SDO）上的极紫外可变性实验（EVE）获得的观测EUV光谱。通过比较拟议模型的计算结果和观察到的EUV光谱数据，我们检查了21个事件的EUV排放的“ EUV耀斑时间积分辐照度”和“ EUV耀斑线上升时间”。所提出的模型成功地再现了Fe VIII 131Å，Fe XVIII 94Å和Fe XX133Å以及55-355Å和55-135Å波段的EUV眩光时间积分辐照度。对于EUV火炬线上升时间，对于所有Fe火炬发射线，建议的模型估计与观测值之间存在可接受的相关性。这些结果表明，所提出的模型可以从具有较高形成温度的发射等离子体再现EUV火炬发射光谱。这表明基于物理学的模型对于精确再现EUV光谱辐照度是有效的。