FRII型射电星系产生的宇宙成因中微子作为超高能事件KM3-230213A的潜在起源
Cosmogenic neutrinos from FRII galaxies as potential origin of the ultra-high-energy KM3-230213A event
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中文总结 AI 辅助
本研究探讨FRII型射电星系瓣加速的UHECR产生的宇宙成因中微子能否解释超高能中微子事件KM3-230213A，通过数值模拟验证其可行性，为该事件起源提供潜在解释并展望多信使观测的研究方向。
中文摘要 AI 辅助
目的：我们研究超高能中微子KM3-230213A是否可被解释为由FRII型射电星系瓣中加速的超高能宇宙射线（UHECR）产生的宇宙成因中微子。方法：我们利用射电星系近期的光度依赖密度演化、射电光度与喷流动能的经验关系，以及FRII瓣UHECR输出的标准假设，模拟了地球处预期的UHECR、宇宙成因中微子和光子通量。FRII对UHECR总体的贡献是从观测到的光度函数自洽推导得出的，而非作为固定归一化值强加。UHECR的传播和次级粒子的产生通过成熟的数值工具计算。结果：预测的宇宙成因中微子通量与从KM3-230213A探测推断出的通量相符，同时与当前UHECR和伽马射线的约束保持一致。根据我们的模型，完整的GRAND天文台（面积200000 km²）应在十年内探测到约50至约135个能量高于10¹⁷ eV的中微子，从而可表征弥散超高能中微子谱。相比之下，探测单个FRII源或与FRII目录的统计显著关联可能仍具挑战性。在最高能量下，UHECR成分和各向异性测量，特别是与近邻射电星系天鹅座A（Cygnus A）相关的测量，应为该情景提供补充检验。更广泛而言，进展可能依赖于多信使观测与FRII型射电星系中粒子加速和喷流成分的改进天体物理约束的结合。
英文摘要
Aim : We investigate whether the ultra-high-energy neutrino KM3-230213A can be interpreted as a cosmogenic neutrino produced by ultra-high-energy cosmic rays (UHECRs) accelerated in the lobes of FRII radio galaxies. Method : We model the UHECR, cosmogenic neutrino and photon fluxes expected at Earth using a recent luminosity-dependent density evolution of radio galaxies, empirical relations between radio luminosity and jet kinetic power, and standard assumptions for the UHECR output of FRII lobes. The FRII contribution to the UHECR population is derived self-consistently from the observed luminosity function, rather than imposed as a fixed normalization. The propagation of UHECRs and the production of secondary particles are computed with well-established numerical tools. Results : The predicted cosmogenic neutrino flux is compatible with that inferred from the detection of KM3-230213A, while remaining consistent with current UHECR and gamma-ray constraints. According to our models, the full GRAND observatory ($200\,000~\rm km^2$) should detect between $\sim50$ and $\sim135$ neutrinos above $10^{17}$~eV in ten years, allowing the diffuse UHE neutrino spectrum to be characterized. In contrast, the detection of individual FRII sources or statistically significant correlations with FRII catalogs is likely to remain challenging. At the highest energies, UHECR composition and anisotropy measurements, in particular those related to the nearby radio galaxy Cygnus~A, should provide complementary tests of this scenario. More generally, progress will likely rely on the combination of multimessenger observations with improved astrophysical constraints on particle acceleration and jet composition in FRII radio galaxies.
