磁陀星 X 射线偏振模型与观测结果
doi: 10.11728/cjss2025.02.2024-0139 cstr: 32142.14.cjss.2024-0139
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陈伟 男, 2000年9月出生于广西壮族自治区北海市, 现为广西大学物理科学与工程技术学院研究生. 主要研究方向为X射线天体物理研究. E-mail: chenwgxu@st.gxu.edu.cn -
谢斐 女, 1989年11月出生于江西省宜春市, 现为广西大学物理科学与工程技术学院教授, 博士生导师, 主要研究方向为X射线偏振探测技术和X射线天体物理研究. E-mail: xief@gxu.edu.cn
作者简介:
通讯作者:
X-ray Polarization Model and Observational Results of Magnetars
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摘要: 磁陀星是磁场高达 1010～1011 T 的中子星, 与普通脉冲星的性质有极大不同. 磁陀星一般与超新星遗迹成协, 存在很强的活动性, 是研究极端天体性质的重要对象, 也是快速射电暴的一种对应体. 磁陀星的磁场结构及活动能量起源一直是磁陀星研究的核心问题, 因此偏振观测信息对理解其性质具有重要意义. 自成像型 X 射线偏振望远镜(IXPE)观测运行以来, 已经对 4U 0142+61, SGR 1806-20, 1RXS J170849.0-400910 和 1E 2259+586 四颗磁陀星进行深度曝光观测, X 射线偏振信息可以加深对磁陀星的认识, 对磁陀星辐射模型做出验证和限制. 本文对这四颗磁陀星的观测结果进行了综合分析, 并将观测结果与主要的磁陀星模型, 即旋转矢量模型、共振康普顿模型和真空共振模型结合进行了讨论.Abstract: Magnetars are a type of neutron star with extremely strong magnetic fields ranging from 1010～1011 T, which are significantly different from the properties of ordinary pulsars. They are generally associated with supernova remnants and exhibit strong activity, making them important objects for studying extreme astrophysical properties and corresponding to one type of Fast Radio Burst (FRB). The magnetic structure and the origin of the activity energy of magnetars have always been central issues in magnetar research, and thus, polarization observation information is crucial for understanding their nature. Since the launch of the Imaging X-ray Polarimetry Explorer (IXPE), in-depth observations have been conducted on four magnetars: 4U 0142+61, SGR 1806-20, 1RXS J170849.0-400910, and 1E 2259+586, marking a deepened study of their properties. This includes the verification and limitation of the magnetar polarization model. This article summarizes the observational results of these four magnetars and discusses the findings in relation to the main magnetar models, which are the rotating vector model, the resonant Compton model, and the vacuum resonance model.
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Key words:
- Magnetar /
- Magnetic Field /
- X-ray polarization
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图 1 光与物质发生光电效应作用截面
Figure 1. Cross-section of the photoelectric effect between light and matter
图 2 脉冲星的模型天球上显示的圆环代表了辐射束的投影. AB 弧线表示视线在天球上形成的投影. 红色实线代表扭曲的偶极场
Figure 2. Pulsar model diagram, where the circle represents the projection of the radiation beam on the celestial sphere. The arc AB is the projection of the line of sight on the celestial sphere. The solid red line represents a twisted dipole field
图 3 在几何参数为 α = 30°, β = 20°, ζ = 65°, 扭曲参数n = 0.5下的偏振位置角随脉冲相位的变化
Figure 3. Variation diagram of the polarization position angle with the pulse phase under the geometric parameters of α = 30°, β = 20°, ζ = 65°and twist parameter n = 0.5
图 4 光子模式的偏振参数(a)和折射率(b)随真空共振附近密度的变化, 其中B =1010 T, E=1 keV, 电子分数 $ {{Y}_{\mathrm{e}}=Z/A=1 }$, 磁场与波矢的夹角 ${ {\theta }_{\mathrm{B}}=45° }$
Figure 4. Polarization parameters (a) and refractive indices (b) of photon modes as functions of density near the vacuum resonance for B =1010 T, E=1 keV, electron fraction $ {{Y}_{\mathrm{e}}=Z/A=1 }$, and the angle between the magnetic field and the wave vector ${ {\theta }_{\mathrm{B}}=45° }$
表 1 IXPE 望远镜的主要性能参
Table 1. IXPE main parameters
参数 数值 工作能段 2～8 keV 视场 (12.9′ )2 角分辨率 < 30″ 能谱分辨率 在 5.9 keV 约为 20% 有效面积 每个探头在 4.5 keV 约为 200 cm2 
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表 2 IXPE 已观测报道的四颗磁陀星的基本信息
Table 2. Basical information about the four magnetars
参数 4U 0142+61 1RXS J170849.0-400910 SGR 1806-20 1E 2259+586 赤经 01h 46m 22s.407 17h 08m 46s.87 18h 08m 39s.337 23h 01m 08s.295 赤纬 +61°45′ 03″ .19 –40°08′ 52″ .44 –20°24′ 39″ .85 +58°52′ 44″ .45 距离/(kpc) 3.6 ± 0.4 3.8 ± 0.5 $ 8.7_{-1.5}^{+1.8} $ 3.2 ± 0.2 磁场/(1010 T) 1.3 4.7 20 0.59 周期/s 8.7 11.0 7.5 7.0 周期导数/(10–11 s·s–1) 0.20 1.95 49.5 0.05 X 射线流量 67.9 24.3 18 ± 1 14.1 ± 0.3 偏振度/(%) 13.5 ± 0.8 [45] 35.1 ± 1.6 [46] 31.6 ± 10.5 [47] 5.6 ± 1.4 [48] 能段/keV 2 ～ 8 2 ～ 8 4 ～ 5 2 ～ 8 注 参数赤经、赤纬、距离、X射线流量信息来源于网站 https://www.physics.mcgill.ca/～pulsar/magnetar/main.html#tab2% , 参数对应参考文献可在网站中进行查阅; 磁场、周期、周期导数信息来自参考文献[10]; 能段为偏振度结果对应能段; kpc为千秒差距. X射线流量单位: 10–15 W·m–2. 流量为2～10 keV能段下, 表格中对应距离下的结果.
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