论文标题
PEVATRON候选人：在X射线带中建模Boomerang星云
A PeVatron Candidate: Modelling the Boomerang Nebula in X-ray Band
论文作者
论文摘要
Pulsar Wind Nebula（PWN）Boomerang和相关的超新星残留（SNR）G106.3+2.7属于Lhaaso发表的超高能量（UHE）Gamma-ray对应物的候选者。尽管扩展来源的质心LHAASO J2226+6057偏离Pulsar的位置约0.3^\ Circ $，但该来源部分覆盖了PWN。因此，我们不能完全排除UHE排放的一部分来自PWN的可能性。先前的研究主要集中于SNR是否是pevatron，同时忽略了能量的PWN。在这里，我们通过研究其X射线辐射来探讨Boomerang Nebula成为Pevatron候选者的可能性。通过建模在PWN中注入的相对论电子的扩散，我们符合X射线表面亮度和光子指数的径向谱。带有磁场$ b =140μ$ g的溶液可以很好地再现观察到的曲线，并意味着严重抑制了电子的IC散射。因此，鉴于最近的Lhaaso对蟹状星云的测量，如果将来的观察结果揭示了源自PWN的UHE发射的一部分，则需要引入质子成分来解释UHE发射。从这个意义上讲，回旋镖星云将是一个耐药的pevatron。
Pulsar wind nebula (PWN) Boomerang and the associated supernova remnant (SNR) G106.3+2.7 are among candidates for the ultra-high-energy (UHE) gamma-ray counterparts published by LHAASO. Although the centroid of the extended source, LHAASO J2226+6057, deviates from the pulsar's position by about $0.3^\circ$, the source partially covers the PWN. Therefore, we cannot totally exclude the possibility that a part of the UHE emission comes from the PWN. Previous studies mainly focus on whether the SNR is a PeVatron, while neglecting the energetic PWN. Here, we explore the possibility of the Boomerang Nebula being a PeVatron candidate by studying its X-ray radiation. By modelling the diffusion of relativistic electrons injected in the PWN, we fit the radial profiles of the X-ray surface brightness and the photon index. The solution with a magnetic field $B=140μ$G can well reproduce the observed profiles and implies a severe suppression of IC scattering of electrons. Therefore, a proton component need be introduced to account for the UHE emission, in light of recent LHAASO's measurement on Crab Nebula, if future observations reveal part of the UHE emission originating from the PWN. In this sense, Boomerang Nebula would be a hadronic PeVatron.
