发表机构
National Technical University of Ukraine, Igor Sikorsky Kyiv Polytechnic Institute（乌克兰国立技术大学，伊戈尔·西科尔斯基基辅理工学院）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本文提出黎曼映射算子（RMO）逆向诊断框架，用于从太阳亮度前沿观测中识别磁流体动力学激波族，通过守恒定律和特征条件测试候选连接，并在多个太阳事件中验证其有效性。
AI 中文摘要
从移动的太阳亮度前沿识别激波，需要将观测到的辐射与等离子体状态的变化联系起来。黎曼框架将激波、稀疏波和其他波描述为连接不同状态的模式的一部分。我们提出了黎曼映射算子（RMO），一种逆向诊断框架，以网络应用程序的形式实现，帮助观测者从不完整的测量中识别磁流体动力学（MHD）激波族。RMO 在保留观测不确定性和模型假设的同时，针对守恒定律、熵要求和特征条件测试候选的局部连接。我们通过五个太阳实例和一项补充的就地比较来演示该方法。一个结合了极紫外（EUV）成像和光谱学的事件，在所测试的条件下同时允许快激波和慢激波连接。对于一个 EUV-射电事件，我们推导出一个上游流约束，该约束在采用模型内将排除普通的慢激波，前提是两个诊断都采样同一前沿。一个耀斑环基准重现了已发表的谱轮廓，并在等温极限中恢复了慢激波排序。太阳轨道器比较恢复了测量速度与磁场变化之间的阿尔芬关系。总之，这些例子展示了 RMO 如何将观测与可接受的 MHD 解释联系起来，并识别出区分它们所需的额外测量。
英文摘要
Identifying a shock from a moving solar brightness front requires relating the observed emission to changes in the plasma state. The Riemann framework describes shocks, rarefactions and other waves as parts of a pattern connecting different states. We present the Riemann Map Operator (RMO), an inverse diagnostic framework implemented as a web application to help observers identify magnetohydrodynamic (MHD) shock families from incomplete measurements. RMO tests candidate local connections against conservation laws, entropy requirements and characteristic conditions, while retaining observational uncertainties and model assumptions. We demonstrate the approach with five solar examples and a complementary in-situ comparison. An event combining extreme-ultraviolet (EUV) imaging and spectroscopy admits both fast and slow shock connections within the tested conditions. For an EUV-radio event, we derive an upstream-flow constraint that would exclude ordinary slow shocks within the adopted model, provided both diagnostics sample the same front. A flare-loop benchmark reproduces the published spectral profiles and recovers slow-shock ordering in the isothermal limit. The Solar Orbiter comparison recovers an Alfvenic relation between measured velocity and magnetic-field changes. Together, the examples show how RMO connects observations to admissible MHD interpretations and identifies the additional measurements needed to distinguish them.
Comments35 pages, 10 figures. Submitted to Solar Physics
