发表机构
University of Chicago; Korea Advanced Institute of Science and Technology (KAIST); Institute for Basic Science; Academia Sinica; National Center for Theoretical Sciences; Kyungpook National University（芝加哥大学; 韩国科学技术院; 基础科学研究院; 中央研究院; 国家理论科学中心; 庆北国立大学）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
提出利用超新星星周介质中511 keV谱线探测微弱相互作用粒子，以暗光子为基准计算信号，并指出与多波长转变的关联特征。
AI 中文摘要
核心坍缩超新星（CCSNe）是微弱相互作用粒子（FIPs）的强烈源，这些粒子在恒星包层之外的可见衰变可以产生独特的电磁信号。我们提出将CCSNe前身星周围的星周介质（CSM）作为511 keV谱线搜索的新目标。逃逸出恒星内部的FIPs可能衰变为电子-正电子对，并将正电子注入CSM中，正电子在其中减速后湮灭，产生511 keV谱线，作为超新星激波突破的电磁前兆。以暗光子为基准模型，我们计算了由SN 2023ixf和SN 2024ggi启发的CSM轮廓的时间相关信号。对于距离10 kpc的银河系超新星，COSI和AMEGO的预期探测能力在部分MeV尺度暗光子参数空间内超越了现有的超新星限制。相同的FIP衰变可以同时加热CSM并使星周尘埃升华，产生从红外过剩到光学或紫外发射的快速光谱转变[Y. Cheng等人，Phys. Rev. Lett. 137, 111005 (2026)]。这种转变与511 keV谱线的同时出现将为致密前超新星环境中FIP衰变提供一种独特的关联多波长特征。
英文摘要
Core-collapse supernovae (CCSNe) are intense sources of feebly interacting particles (FIPs), whose visible decays beyond the stellar envelope can generate distinct electromagnetic signals. We propose the circumstellar medium (CSM) surrounding the CCSNe progenitor as a new target for 511 keV line searches. FIPs escaping the stellar interior may decay into electron-positron pairs and inject positrons into the CSM, where they slow down and subsequently annihilate, giving rise to a 511 keV line as an electromagnetic precursor to the supernova shock breakout. Using dark photons as a benchmark, we calculate the time-dependent signal for CSM profiles motivated by SN 2023ixf and SN 2024ggi. For a Galactic supernova at 10 kpc, the projected reach of COSI and AMEGO extends beyond existing supernova limits over part of the MeV-scale dark-photon parameter space. The same FIP decays can simultaneously heat the CSM and sublimate circumstellar dust, producing a rapid spectral transition from infrared excess to optical or ultraviolet emission [Y. Cheng et al., Phys. Rev. Lett. 137, 111005 (2026)]. The coincident appearance of this transition and the 511 keV line would provide a distinctive correlated multiwavelength signature of FIP decays in the dense presupernova environment.
Comments10+1 pages, 5+3 figures, 125 references
