发表机构
ASTRON, the Netherlands Institute for Radio Astronomy; Institute of Space Sciences (CSIC-ICE); Institut d’Estudis Espacials de Catalunya (IEEC); Department of Physics, Royal Holloway, University of London; Departament de Física, Universitat d’Alacant（荷兰射电天文研究所; 空间科学研究所; 加泰罗尼亚太空研究学院; 伦敦大学皇家霍洛威学院物理系; 阿利坎特大学物理系）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究通过模拟推断方法构建统一演化框架，重现三类孤立中子星的辐射，确定其诞生磁场分布与诞生率，助力明确中子星作为高能瞬变现象中心引擎的贡献。
AI 中文摘要
在统一框架下理解银河系孤立中子星的种群，可为其诞生属性、演化路径及不同中子星类别间的关联提供关键见解。本研究旨在重现观测到的孤立中子星的射电与宁静X射线辐射，包括射电脉冲星、磁星和X射线暗弱孤立中子星（XDINSs）。我们开发了一个综合种群合成框架，该框架模拟中子星的诞生属性、动力学、自转、磁热演化，以及射电与X射线辐射，还有对应巡天的选择效应。为模拟真实的X射线光谱，我们考虑了磁层共振回旋散射和星际吸收。此外，我们通过将磁星的爆发率与恒星壳层的磁应力关联，来模拟磁星爆发引入的观测偏差。随后，我们采用一种名为截断序列神经后验估计的模拟推断方法，重建诞生属性，如初始磁场分布。我们发现银河系中子星种群可由诞生磁场的双组分对数正态分布描述，峰值分别为5×10¹²高斯和10¹⁴高斯。我们还发现银河系中子星的诞生率约为每世纪3至4次。我们的结果有助于确立中子星作为快速射电暴、超亮超新星和伽马射线暴等高能天文瞬变现象中心引擎的贡献。
英文摘要
Understanding the Galactic population of isolated neutron stars within a unified framework provides key insights into their birth properties, evolutionary pathways, and the connections between different neutron star classes. In this work, we aim to reproduce both the observed radio and quiescent X-ray emission from isolated neutron stars, including radio pulsars, magnetars and X-ray dim isolated neutron stars (XDINSs). We develop a comprehensive population synthesis framework that models neutron star birth properties, their dynamical, rotational, and magneto-thermal evolution, as well as radio and X-ray emission, and the selection effects of corresponding surveys. To simulate realistic X-ray spectra, we account for magnetospheric resonant cyclotron scattering and interstellar absorption. Additionally, we model the observational bias introduced by magnetar outbursts, by linking the outburst rate to magnetic stresses in the stellar crust. We then employ a simulation-based inference method, namely truncated sequential neural posterior estimation, to reconstruct the birth properties, such as the initial magnetic field distribution. We find that the Galactic neutron star population can be described by a two-component log-normal distribution of birth magnetic fields with peaks at $5 \times 10^{12}$ G and $10^{14}$ G, respectively. We further find that the Galactic neutron star birth rate is around 3-4 per century. Our results help establish the contribution of neutron stars as central engines of powerful astrophysical transient phenomena, such as fast radio bursts, super-luminous supernovae and gamma ray bursts.
Comments33 pages, 16 figures, 2 tables, accepted by ApJ
