标题： 通过伽马射线和中微子对应关系探测LHAASO银河PeVatron 显示英文标题

标题： Probing LHAASO Galactic PeVatrons through gamma-ray and neutrino correspondence

摘要： 最近，大型高海拔空气簇射观测站（LHAASO）已经检测到几个银河系的超高能（UHE；$E_{\gamma}> 100$TeV）伽马射线点源。 这些伽马射线可能是在拍电子伏特能量宇宙射线（CRs）的轻子或强子相互作用中产生的。 在强子通道（$p-p$相互作用）中，伽马射线伴随着中微子。 因此，中微子的探测对于理解此类天体中的宇宙射线加速至关重要。 为了估计中微子通量，我们采用了两个LHAASO源（J2226+6057，J1908+0621），这两个源被发现与超新星遗迹（SNR G106.3+2.7，SNR G40.5-0.5）在空间上相关。 对于这两个源，检测到的TeV-PeV伽马射线谱被发现异常硬（光谱指数$\sim$1.8）。 我们基于上述两个原型建立了伽马射线和中微子辐射模型。 从这两个源产生的中微子通量低于IceCube的灵敏度，但在即将进行的IceCube-Gen2和KM3NeT实验中是可以探测到的。 我们进一步估计了其他10个类似LHAASO PeVatron源的中微子通量，其中大部分在IceCube-Gen2和KM3NeT中是可以探测到的。 最后，我们探讨了我们的模型参数，特别是光谱幂律指数，并评估了中微子探测器在未来探测此类银河系源中宇宙射线加速的潜力。 显示英文摘要

摘要： Recently, Large High Altitude Air Shower Observatory (LHAASO) has detected several Galactic point sources of ultra high energy (UHE; $E_{\gamma}> 100$ TeV) gamma-rays. These gamma-rays are possibly created in leptonic or hadronic interactions of cosmic rays (CRs) of PeV energies. In the hadronic channel ($p-p$ interaction), the gamma-rays are accompanied by neutrinos. The detection of neutrinos is therefore crucial in understanding CR acceleration in such objects. To estimate the neutrino flux, we adopt the two LHAASO sources (J2226+6057, J1908+0621) found to be spatially associated with the Supernova remnants (SNR G106.3+2.7, SNR G40.5-0.5). For these two sources, the detected TeV-PeV gamma-ray spectra are found to be unusually hard (with spectral index $\sim$ 1.8). We develop a model of gamma-ray and neutrino emission based on the above two prototypes. The neutrino fluxes from these two sources are found to be below the IceCube sensitivity, but are detectable in upcoming IceCube-Gen2 and KM3NeT experiments. We further estimate the neutrino fluxes from similar other 10 LHAASO PeVatron sources and most of them are found to be detectable in IceCube-Gen2 and KM3NeT. Finally, we explore our model parameters, in particular the spectral power law index and estimate the future potential of the neutrino detectors to probe CR acceleration in such Galactic sources.