发表机构
Ariel University; Istituto Nazionale di Fisica Nucleare, Sezione di Roma; INAF - Istituto di Radioastronomia（阿里埃尔大学; 意大利国家核物理研究所罗马分部; 意大利国家天体物理研究所射电天文台）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究提出数据驱动框架，利用X射线吸收柱密度和激波速度重建CSM分布，预测SN 2023ixf和SN 2024ggi的中微子发射，并确定最佳探测时间窗口。
AI 中文摘要
与稠密星周介质（CSM）相互作用的核坍缩超新星（CCSNe）是高能中微子的有前景的来源。大多数中微子预测依赖于对CSM密度分布和前身星质量损失历史的特定假设。我们开发了一个数据驱动的框架，将X射线观测直接与预期中微子信号联系起来。利用氢等效吸收柱密度N_H(t)的时间演化，结合由X射线等离子体温度推断出的激波速度，我们重建了CSM密度分布和激波速度演化。我们估计了激波突破（SBO）时期及由此产生的中微子发射，并将该方法应用于邻近相互作用超新星SN 2023ixf和SN 2024ggi。对于这两个源，我们计算了IceCube和KM3NeT/ARCA的预期中微子事件率。我们发现中微子产生集中在SBO附近，此时强子相互作用最为有效。这自然地定义了一个每个源特有的短时间窗口，可最大化信噪比。我们的结果表明，X射线观测可以同时约束预期中微子信号及其探测的最佳时间窗口，为这些激波驱动的暂现源的多信使搜索提供了一种观测驱动的策略。
英文摘要
Core-collapse supernovae (CCSNe) interacting with a dense circumstellar medium (CSM) are promising sources of high-energy neutrinos. Most neutrino predictions rely on specific assumptions about the CSM density profile and progenitor mass-loss history. We develop a data-driven framework that connects X-ray observations directly to the expected neutrino signal. Using the temporal evolution of the hydrogen-equivalent absorbing column density, N_H(t), together with the shock velocity inferred from the X-ray plasma temperature, we reconstruct the CSM density profile and shock velocity evolution. We estimate the shock-breakout (SBO) epoch and the resulting neutrino emission, and apply the method to the nearby interacting supernovae SN 2023ixf and SN 2024ggi. For both sources, we compute the expected neutrino event rates for IceCube and KM3NeT/ARCA. We find that neutrino production is concentrated near SBO, when hadronic interactions are most efficient. This naturally defines a short time window, specific to each source, that maximizes the signal-to-background ratio. Our results demonstrate that X-ray observations can constrain at once both the expected neutrino signal and the optimal time window for its detection, providing an observationally-driven strategy for multimessenger searches of these shock-powered transients.
