脉冲星双星的制动指数研究

发布时间：2018-03-17 22:00

本文选题：脉冲星　切入点：双星系统　出处：《华中科技大学》2016年硕士论文　论文类型：学位论文

【摘要】：脉冲星高速旋转的中子星,其极端的物理条件如高密度、高温度、高磁场、高速旋转等可以帮助我们了解致密星体的物理构成。脉冲双星系统的精确的到达时间测量,可以使我们检验广义相对论和其它引力理论给出的不同预言。本论文围绕脉冲双星系统中脉冲星制动指数的异常展开。观测数据显示了脉冲双星系统的制动指数远大于单个脉冲星的指制动数。我们认为脉冲双星系统中多普勒残余引起的时间残差可以影响脉冲双星的频率一阶导数和二阶导数从而使得脉冲双星的制动指数远大于3。该研究在脉冲星的理论和应用研究方面具有重要意义。理解脉冲星的自转减慢机制,可以使我们更加了解脉冲星到达时间残差的起因。从而为利用脉冲星到达时间检验广义相对论性预言的引力波、以及脉冲星导航等创造更加好的条件。论文分为六章。第一章综述了脉冲星及研究的基本问题,内容包括脉冲星的内部结构,物态方程,质量半径关系。介绍了典型的脉冲星辐射区。第二章对脉冲星制动指数进行介绍,对脉冲星的能量来源,自转减慢进行探讨。按经典的磁偶极辐射模型,脉冲星的制动指数应该等于3。然而根据脉冲双星的自转频率和自转频率的一阶导数和二阶导数,得出的制动指数往往远大于3。第三章介绍脉冲双星系统到达时间测量模型,对脉冲星到达时间处理软件Tempo2进行介绍。观测者接收到的脉冲星信号往往存在时间残差。第四章研究21颗脉冲双星系统的制动指数。通过引入脉冲星在轨道运动中的多普勒残余效应对自转频率一阶导数的贡献,使得自转频率的一阶导数减小,进而使得这些脉冲双星的制动指数大幅度减小。结果21颗脉冲双星中的绝大部分脉冲星的制动指数从十的四、五次方等降到了3左右。并结合轨道-自旋耦合模型和伴星引起的测地进动轨道进动模型,对剩余的修正后的脉冲星制动指数进一步分析。第五章是将多普勒残余效应移植到脉冲双星到达时间处理软件Tempo2。在多普勒效应引起的自转频率一阶导数的变化导致的时间残差不被忽略的情况下,所得到的时间残差和不考虑脉冲双星系统中多普勒残余效应得到的时间残差进行比较,在两颗脉冲星的到达时间残差降低或者不变的情况下,使脉冲星制动指数降到正常值。第六章是总结和展望。此部分总结了脉冲双星系统中多普勒残余效应对脉冲双星到达时间的影响,解释了21颗脉冲双星制动指数异常的问题。并对两颗有到达时间观测数据的脉冲双星在Tempo2里实现了使制动指数降到了正常。
[Abstract]:The extreme physical conditions such as high density, high temperature, high magnetic field, high speed rotation and so on can help us to understand the physical composition of dense stars. This paper focuses on the anomaly of pulsar braking index in pulsating binary system. The observed data show the braking exponent of pulsating binary system. We think that the time residuals caused by Doppler residue in pulsating binary system can affect the first derivative and second derivative of the frequency of pulsating binary stars, thus making the braking index of pulsating binary stars. This study is of great significance in the theoretical and applied studies of pulsars. It is possible to understand better the cause of the pulsar arrival time residuals, so as to test the gravitational waves of the generalized relativistic prophecy by using the pulsar arrival time. The thesis is divided into six chapters. The first chapter summarizes the pulsar and its basic problems, including the internal structure of pulsar, the equation of state, The relation of mass radius. The typical emitter region of pulsar is introduced. In the second chapter, the braking index of pulsar is introduced, the energy source of pulsar, the slow rotation of pulsar are discussed. According to the classical magnetic dipole radiation model, The braking index of pulsar should be equal to 3. However, according to the first and second derivative of rotation frequency and rotation frequency of pulsating binary star, the braking index is often greater than 3. In chapter 3, the measurement model of arrival time of pulsating binary satellite system is introduced. The time of arrival processing software Tempo2 is introduced. The pulsar signals received by observers often have time residuals. In chapter 4th, the braking index of 21 pulsar binary systems is studied. The pulsar motion in orbit is introduced by introducing pulsars. The contribution of Doppler residual effect to the first derivative of rotation frequency, The first derivative of rotation frequency is reduced, and the braking index of these two pulsars is greatly reduced. As a result, the braking index of most of the 21 pulsating binary stars is from four to ten. The fifth power is reduced to about 3. Combined with the orbital spin-spin coupling model and the geodesic precession model caused by the companion star, Further analysis of the remaining modified pulsar braking index. Chapter 5th is to transplant the Doppler residual effect to the pulsar arrival time processing software Tempo2. The variation of the first derivative of the rotation frequency caused by the Doppler effect. If the resulting time residuals are not ignored, The time residuals obtained are compared with the time residuals obtained without considering the Doppler residual effect in the pulse binary system. When the arrival time residuals of the two pulsars decrease or remain unchanged, The braking index of pulsar is reduced to the normal value. Chapter 6th is a summary and prospect. In this part, the influence of Doppler residual effect on arrival time of pulsating binary stars is summarized. In this paper, the problem of abnormal braking index of 21 binary pulsating stars is explained, and the braking index is reduced to normal in Tempo2 for two pulsed binary stars with time of arrival observation.
【学位授予单位】：华中科技大学
【学位级别】：硕士
【学位授予年份】：2016
【分类号】：P145.6

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