作为超高能强子发射诊断的蟹状星云能量相关延展
Energy-dependent extension of the Crab Nebula as a diagnostic of ultrahigh-energy hadronic emission
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中文总结 AI 辅助
本研究提出蟹状星云能量相关延展可作为脉冲星风星云中超高能伽马射线起源的判别器，通过空间分辨轻子-强子场景解释其与轻子预期的差异，发现400 TeV以上强子主导、1.1 PeV处包含半径为纯轻子场景6倍，实现PeV强子加速诊断。
中文摘要 AI 辅助
蟹状星云的能量相关表观延展与X射线和TeV波段的轻子预期不符，可在空间分辨的轻子-强子场景中自然解释。在约400 TeV以上发生向强子主导的转变，PeV能量下几乎为纯强子发射。1.1 PeV处预测的68%包含半径约为1.4角分，约为纯轻子场景的6倍。因此，这种能量相关延展可作为脉冲星风星云中超高能伽马射线发射起源的可观测判别器，为蟹状星云的PeV强子加速提供诊断手段。
英文摘要
The energy-dependent apparent extension of the Crab Nebula, inconsistent with leptonic expectations between X-ray and TeV bands, can be naturally accounted for in a spatially resolved lepto-hadronic scenario. A transition to hadronic dominance occurs above $\sim400~\rm{TeV}$, with nearly pure hadronic emission at PeV energies. The predicted $68\%$ containment radius at $1.1~\rm{PeV}$ is $\sim1.4'$, about six times larger than in purely leptonic scenarios. This energy-dependent extension therefore provides an observable discriminator of the origin of ultra-high-energy gamma-ray emission in pulsar wind nebulae, offering a diagnostic of PeV hadronic acceleration in the Crab Nebula.
