低质量X射线双星中的吸积中子星
Accreting Neutron Stars in Low-Mass X-ray Binaries
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中文总结 AI 辅助
本文综述低质量X射线双星中吸积中子星的研究，调查相关系统类别，研究I型X射线暴、吸积流物理，结合IXPE偏振结果等提供发射区域几何结构的新约束。
中文摘要 AI 辅助
中子星低质量X射线双星（NS LMXBs）是一类系统，其中中子星通过吸积盘从充满洛希瓣的伴星吸积物质，释放的引力能量效率约为静能的10%-20%。与黑洞不同，中子星拥有固体表面和磁场，这使得NS LMXBs成为高能天体物理学和致密物质物理学领域独特且丰富的实验室。在本章中，我们综述了当前对LMXBs中中子星吸积过程的理解，追踪物质从外吸积盘半径到恒星表面的过程，覆盖了五十年的观测发现。我们调查了主要的吸积中子星系统类别——经典的atoll源和Z源、超紧凑型X射线双星、吸积毫秒脉冲星以及过渡型毫秒脉冲星，并讨论它们的谱态、时变特性和多波段行为如何编码内吸积流的物理信息。我们研究了热核I型X射线暴作为核燃烧和中子星结构的探针，并综述了吸积物质减速到恒星表面的边界层和扩散层。我们讨论了相对论性喷流和电离盘风作为吸积-喷流循环的调控因素。最后，我们展示了来自成像X射线偏振探测器（IXPE）的X射线偏振结果，这些结果首次提供了虽依赖模型但新的约束，涉及发射区域（吸积盘、冕、扩散层和喷流）的几何结构，这些是仅靠光谱学无法分辨的，同时还有互补的光学和红外偏振观测。
英文摘要
Neutron star low-mass X-ray binaries (NS LMXBs) are systems in which a neutron star accretes matter from a Roche-lobe-filling companion via an accretion disc, releasing gravitational energy with an efficiency of order 10-20% of the rest-mass energy. Unlike black holes, neutron stars possess a solid surface and a magnetic field, making NS LMXBs uniquely rich laboratories for high-energy astrophysics and dense-matter physics. In this chapter we review the current understanding of accretion onto neutron stars in LMXBs, tracing matter from the outer disc radii to the stellar surface across five decades of observational discovery. We survey the principal classes of accreting neutron star systems - canonical atoll and Z-sources, ultracompact X-ray binaries, accreting millisecond pulsars, and transitional millisecond pulsars - and discuss how their spectral states, timing properties, and multiwavelength behaviour encode the physics of the inner accretion flow. We examine thermonuclear Type-I X-ray bursts as probes of nuclear burning and neutron star structure, and review the boundary and spreading layers where accreted matter decelerates onto the stellar surface. We discuss relativistic jets and ionised disc winds as regulators of the accretion-ejection cycle. Finally, we present X-ray polarimetric results from the Imaging X-ray Polarimetry Explorer (IXPE), which for the first time provide new, though model-dependent, constraints on the geometry of the emission regions - disc, corona, spreading layer, and jets - that spectroscopy alone cannot resolve, alongside complementary optical and infrared polarimetric observations.
发表机构
- INAF–Osservatorio Astronomico di Brera（意大利国家天体物理研究所布拉拉天文台）
- University of Turku（图尔库大学）
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