快速转动磁星供能的暂现源研究

Rapidly-rotating magnetars as ultra-highly magnetic pulsars are not only of great importance for studying physical processes under extreme conditions, but their formation and evolution also can drive different kinds of multi-wavelength transients and maybe produce strong gravitational wave signals. The existing observations and theoretical studies have shown that rapidly-rotating magnetars are very likely to be central engines of some gamma-ray burst afterglows, electromagnetic bursts induced by mergers of double neutron stars, and superluminous supernovae. Combining observed data of the Swift and Fermi satellites with ground-based optical and radio telescopes, (1) we will study the plateaus of gamma-ray burst afterglows, electromagnetic bursts induced by mergers of double neutron stars and superluminous supernovae, explain them by considering the rapidly-rotating magnetar-powered model, and obtain constraints on the newborn magnetar properties; (2) we will study the dissipation mechanism and efficiency of the magnetar's spinning energy; (3) we will study the evolution of the spin, magnetic field, and mass to obtain both information on gravitational waves and constraints on the equations of state for neutron matter; (4) we will propose a unified model for the magnetar-powered and radioactive decay-powered mechanisms and explain some special transients; (5) we will analyze the observed data of superluminous supernovae to obtain a Phillips- like relation and to provide a theoretical explanation for this relation.

快速转动磁星作为超强磁场的脉冲星不仅对于研究极端条件下物理过程有非常重要的意义，而且它们可以驱动不同类型的多波段暂现源，甚至可能产生很强的引力波辐射信号。现有的观测和理论研究表明快速转动磁星很可能是部分伽玛暴余辉、双中子星并合引起的电磁暴、超亮超新星等暂现源的中心引擎。结合空间Swift和Fermi等卫星以及地面光学和射电望远镜对暂现源的观测数据，本项目将（1）研究伽玛暴余辉平台、双中子星并合引起的电磁暴、超亮超新星，并用快速转动磁星供能模型给出理论解释，从而获得对初生磁星物理参量的限制；（2）研究磁星的转动能耗散机制及其效率；（3）研究磁星的自旋、磁场和质量的演化，获得引力波辐射信息以及对中子物质状态方程的限制；（4）提出描述磁星供能和放射线重元素衰变供能的统一模型，并试图在该模型框架下解释特殊的暂现源；（5）分析超亮超新星的观测数据，试图得到标准烛光关系，并用磁星供能模型给出理论解释。

本项目主要针对快速射电暴的起源和辐射机制、GW170817的电磁对应体、伽玛暴余辉平台、超量超新星等课题进行了系列研究，取得了许多重要研究成果。这些现象的中心引擎是强磁场毫秒脉冲星。本项目提出了重复快速射电暴的脉冲星-小行星带碰撞模型和非重复暴的双中子星并合模型，分析了最亮超量超新星的中心引擎脉冲星参数并建议它可能是奇异夸克星，用MCMC方法拟合了一批超亮超新星并得到磁星的物理参数，研究了毫秒磁星的相对论星风的磁耗散机制并发现星风的X射线辐射效率与自转减慢光度相关，计算了双中子星并合后的径向振荡脉冲星的引力波辐射并发现将来的引力波探测器可能会探测到这类引力波辐射，研究了转动黑洞-磁化中子星的并合，发现了此类并合可能会产生短伽玛暴和快速射电暴, 等等。本项目共发表SCI论文70篇，其中绝大数论文都是在ApJ Letters、ApJ、MNRAS、A&A、Physical Review D等国际天文一流核心刊物上发表。