关于脉冲星线偏振位置角与辐射几何研究的评述  

A review of the study on linear polarization position angle and emission geometry of pulsars

作　　者：王洪光[1] 郑晖[2] 黄文俊[1] WANG Hong-guang ZHENG Hui HUANG Wen- jun(School of Physics and Electronic Engineering School of Mechanical and Electronical Engineering , Guangzhou University , Guangzhou 510006 , China)

机构地区：[1]广州大学物理与电子工程学院,广东广州510006 [2]广州大学机械与电气工程学院,广东广州510006

出　　处：《广州大学学报（自然科学版）》2017年第2期14-20,共7页Journal of Guangzhou University:Natural Science Edition

基　　金：国家自然科学基金资助项目(11178001;11573008)

摘　　要：脉冲星是快速自转的中子星,其射电辐射往往具有较高的偏振度.20世纪60年代末运用旋转矢量模型拟合线偏振位置角曲线的方法,从中能够得到脉冲星的2个重要辐射几何参数——磁倾角和视线碰撞角.这对研究脉冲星辐射、动力学和演化都非常有用.随后有许多工作研究了不同的物理和几何效应对旋转矢量模型的影响,其中利用光行差效应估算辐射高度的方法得到了广泛的应用.但是这些方法都有理论上的局限性,只适用于辐射高度较低的脉冲星.文章综述了从线偏振位置角中提取辐射几何和辐射区参数的方法,介绍了辐射几何在多个方面研究中的应用,并对前人研究方法中存在的问题以及未来发展方向进行了评述.Pulsars are fastly rotating neutron stars. Most pulsars show strong polarization in tating vector model was proposed in late 1960s and used to constrain two important emission geometry parame-ters ,the magnetic inclination angle and the impact angle between the line of sight and the magnetic axis , by fit-ting the observed linear polarization angles. These parameters are very useful to the studies of pulsar emission ,dynamics and evolution. Many successive studies were performed to revise the classical rotating vector model byconsidering various physical and geometrical effects , among which a method to estimate the considering the aberration effect was developed and widely used. However , these methods have theoretical limi-tations. They are only applicable to pulsars with low emission altitudes. In this paper we reviewed the previous methods to determine the parameters of emission geometry and emission region , and defined their application in a couple of related issues , current problems and the direction of future study.

关 键 词：脉冲星 射电辐射 偏振 辐射几何 

分 类 号：O412.1[理学—理论物理]