Swift J1834.9-0846/W41区域非热辐射的多波长研究
Multiwavelength study of non-thermal emission in the Swift J1834.9-0846/W41 region
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中文总结 AI 辅助
研究Swift J1834-0846/W41区域非热辐射起源，在轻子和轻子-强子框架内建模其光谱能量分布，对比不同情景，发现纯轻子模型不合适，轻子-强子解决方案更合理，模拟观测显示30小时曝光可区分形态并扩展光谱测量。
中文摘要 AI 辅助
我们通过使用马尔可夫链蒙特卡罗采样，在轻子和轻子-强子框架内对Swift J1834-0846/W41区域从射电到TeV能量的宽带光谱能量分布进行建模，来研究其非热辐射的起源。受HESS J1834-087形态学研究的启发，探索了单扩展源情景和包含嵌入扩展发射中的中心点状成分的配置。在两种情景中，纯轻子模型因磁场强度过低而不被青睐，轻子-强子解决方案产生的场强和非热能预算与经历有效宇宙射线加速的演化超新星遗迹一致。在双成分情景中，强子相互作用主导了W41的扩展TeV辐射，而中心过剩由由Swift J1834-0846驱动的轻子磁星风星云很好地描述，这意味着初始自旋周期短，$P_0 \lesssim 0.2$ s。用切伦科夫望远镜阵列天文台进行的模拟观测表明，30小时的曝光将区分两种形态配置，并将光谱测量扩展到超过约10 TeV。
英文摘要
We investigate the origin of non-thermal emission from the Swift J1834-0846/W41 region by modeling its broadband spectral energy distribution from radio to TeV energies within leptonic and lepto-hadronic frameworks using Markov Chain Monte Carlo sampling. Motivated by morphological studies of HESS J1834-087 suggesting a two-component TeV structure, we explore a single extended source scenario and a configuration comprising a central point-like component embedded within extended emission. Purely leptonic models are disfavored in both scenarios by unrealistically low magnetic field strengths, whereas lepto-hadronic solutions yield field intensities and non-thermal energy budgets consistent with an evolved supernova remnant undergoing efficient cosmic-ray acceleration. In the two-component scenario, hadronic interactions dominate the extended TeV emission from W41, while the central excess is well described by a leptonic magnetar wind nebula powered by Swift J1834-0846, implying a short initial spin period of $P_0 \lesssim 0.2$ s. Simulated observations with the Cherenkov Telescope Array Observatory show that 30 h exposures will discriminate between the two morphological configurations and extend spectral measurements beyond $\sim$10 TeV.
