AI 中文总结
研究磁星CXOU J171405.7 - 381031附近非热辐射，用轻子和轻子 - 强子模型结合马尔可夫链蒙特卡罗技术分析多波长数据，对比不同模型表现，模拟CTAO观测，有望约束质子截止能量，测试强子发射。
AI 中文摘要
磁星是具有超强磁场（$B \sim 10^{14}$ - $10^{15}$ G）的中子星，是高能粒子加速的潜在候选者。我们对与超新星遗迹（SNR）CTB 37B相关的磁星CXOU J171405.7 - 381031周围区域进行了多波长分析。利用轻子和轻子 - 强子模型对从射电到TeV能量的宽带光谱能量分布进行建模，通过马尔可夫链蒙特卡罗技术约束粒子种群。在SNR框架内，两种模型都能较好描述伽马射线数据。纯轻子模型能再现整体光谱形状，但略低估H.E.S.S.测量的最高能量通量；轻子 - 强子解释在$\sim 10$ TeV以上能更好描述，GeV发射以逆康普顿散射为主，最高能量处中性π介子衰变有贡献。若遗迹与致密环境介质相互作用，所需质子能量（$W_{\rm p} \gtrsim 10^{51}$ erg）可大幅降低。磁星风星云模型能再现宽带光谱，但与观测到的源形态强烈不符。模拟切伦科夫望远镜阵列天文台（CTAO）观测表明，约50小时的曝光将约束质子截止能量，从而对该区域的强子发射进行决定性测试。
英文摘要
Magnetars are neutron stars with ultra-strong magnetic fields ($B \sim 10^{14}$-$10^{15}$ G) and are promising candidates for high-energy particle acceleration. We present a multiwavelength analysis of the region surrounding CXOU J171405.7-381031, a magnetar associated with the supernova remnant (SNR) CTB 37B. The broadband spectral energy distribution spanning radio to TeV energies is modeled using leptonic and lepto-hadronic scenarios, with particle populations constrained using Markov Chain Monte Carlo techniques. Within an SNR framework, both scenarios provide acceptable descriptions of the gamma-ray data. The purely leptonic model reproduces the overall spectral shape but slightly underestimates the highest-energy flux measured by H.E.S.S., whereas a lepto-hadronic interpretation offers an improved description above $\sim 10$ TeV, with inverse-Compton scattering dominating the GeV emission and neutral-pion decay contributing at the highest energies. The required proton energy ($W_{\rm p} \gtrsim 10^{51}$ erg) can be substantially reduced if the remnant interacts with a dense ambient medium. A magnetar wind nebula scenario can reproduce the broadband spectrum but is strongly disfavored by the observed source morphology. Simulated Cherenkov Telescope Array Observatory (CTAO) observations indicate that exposures of $\sim 50$ h will constrain the proton cut-off energy, enabling a decisive test of hadronic emission in this region.
CommentsAccepted for publication in MNRAS
