脉冲星PSR B1259-63的极冠几何结构研究
发布时间：2018-11-12 07:03
【摘要】：本文内容涉及作者在硕士生阶段的研究工作,包括对短时标暂现射电现象观测研究进展的探讨和对脉冲星PSR B1259-63极冠几何结构的研究。主要研究工作是在确定脉冲星磁倾角α以及视线方向与磁轴之间的夹角β的计算上,这两个参量是表征脉冲星辐射锥特性的重要物理量,不能由观测直接给出,只能由极冠模型的几何研究和统计分析来获得。这两个参量值的确定对脉冲星的磁层结构和辐射机制的确立都有重要意义。 本文第二章介绍了目前国内外对短时标暂现射电现象观测研究进展方面的讨论,短时标暂现射电源(RRATs)是一类特殊的射电源,与普通脉冲星相比,它具有以下的特征:发射稀少的毫秒级时标的爆发式射电脉冲,发射期内脉冲没有周期性,即每次只发射一个单独的射电脉冲,所以探测这类射电源非常困难。目前共发现大约46个这种类型的短时标暂现射电源,其中大约27个已确定了它们有秒级自转周期,7个源测得了周期导数。本章主要介绍这7个已测得周期导数的短时标暂现射电源的一些性质及它们与其它已知的几类中子星的关系与区别。 本文第三章介绍了对脉冲星PSR B1259-63极冠几何结构的研究。本章利用欧洲脉冲星观测网(EPN)数据库里PSR B1259-63在1.52GHz、4.68GHz和8.28GHz三个频率上的线偏振位置角观测数据研究这颗脉冲星可能的极冠几何结构。本研究分别假设了PSR B1259-63是平行转子和垂直转子两种情况,用脉冲星旋转矢量模型(RVM)对线偏振位置角观测数据进行了最小二乘法拟合研究。在平行转子假设下,对三个频率观测结果拟合得到了两套可能的模型(a、b)参数,模型(a)的α=10.0~0±0.5~0、β=0.5~0±0.3~0,模型(b)的α=36.3~0±2~0、β=9~0±2~0,这与Manchester和Johnston在1995年得到的结果基本一致。在垂直转子假设下,对三个频率观测的主脉冲(MP)和中间脉冲(IP)数据拟合得到两个磁极参数分别为αMP=83~0±2~0、βMP=-3~0±1~0和αIP=97~0±1~0、βIP=-17~0±1~0,表明主脉冲和中间脉冲可能分别源自脉冲星两个磁极,不能排除该星是垂直转子的可能性。目前的观测数据还不能明确限定PSR B1259-63的极冠几何结构,有必要进行更深入的观测与研究。 在第四章里总结了本文的工作。
[Abstract]:This paper deals with the author's research work in the master stage, including the investigation of the observation progress of short-time scale temporary radio phenomena and the study of the geometric structure of the pulsar PSR B1259-63. The main research work is to determine the calculation of the pulsar's magnetic dip angle 伪 and the angle 尾 between the direction of sight and the magnetic axis. These two parameters are important physical quantities to characterize the characteristics of the pulsar's radiating cone, and cannot be directly given by observation. It can only be obtained from the geometric study and statistical analysis of the polar crown model. The determination of these two parameters is of great significance to the establishment of magnetosphere structure and radiation mechanism of pulsars. In the second chapter of this paper, the recent research progress in the observation of short-time scale temporary radio is introduced. The short-time temporary radio source (RRATs) is a special radio source, compared with the ordinary pulsar. It has the following characteristics: it emits a few milliseconds of targeted explosive radio pulses, and the pulse has no periodicity during the emission period, that is, only one single radio pulse is transmitted at a time, so it is very difficult to detect this kind of radio source. At present, about 46 short-time temporary radio sources of this type have been found, of which about 27 have determined that they have a rotation period of second order, and 7 sources have measured periodic derivatives. In this chapter, some properties of these seven short-time scale temporary radio sources with measured periodic derivatives and their relationship with other known neutron stars are introduced. In the third chapter, the geometrical structure of PSR B 1259-63 polar crowns is studied. In this chapter, the possible polar crown geometry of the pulsar is studied by using the linear polarization position angle data of PSR B1259-63 at 1.52GHz 4.68GHz and 8.28GHz in the (EPN) database of the European Pulsar Observatory. In this study, we assume that PSR B1259-63 is a parallel rotor and a vertical rotor, and use the pulsar rotation vector model (RVM) to fit the linear polarization angle data by least square method. Under the assumption of parallel rotors, two sets of possible model parameters (AGB) were obtained by fitting the three frequency observations. The model (a) 伪 = 10.0 卤0.5 0, 尾 = 0.5 0 卤0.3 0, model (b) 伪 = 36.33 卤2 0, 尾 = 9 0 卤2.0, respectively, and a = 0 0 卤0 0, 尾 = 10 0 卤0 0, 尾 = 0 0 卤0 0, respectively, for model (b), 伪 = 36. 3 卤2. 0, 尾 = 9. 0 卤2. 0, respectively. This is basically consistent with the results obtained by Manchester and Johnston in 1995. On the assumption of vertical rotor, the main pulse (MP) and intermediate pulse (IP) data of three frequencies were fitted to obtain two magnetic pole parameters: 伪 MP=83~0 卤2 0, 尾 MP=-3~0 卤1 0 and 伪 IP=97~0 卤1 0, 尾 IP=-17~0 卤1 0, respectively, and the two magnetic pole parameters are 伪 MP=83~0 卤2 0, 尾 MP=-3~0 卤1 0 and 伪 IP=97~0 卤1 0, 尾 IP=-17~0 卤1 0, respectively. It is shown that the main pulse and the intermediate pulse may originate from the two poles of the pulsar respectively, and the possibility that the star is a vertical rotor can not be ruled out. The current observational data cannot clearly define the polar crown geometry of PSR B1259-63, so it is necessary to make further observation and study. In the fourth chapter, the work of this paper is summarized.
【学位授予单位】：新疆大学
【学位级别】：硕士
【学位授予年份】：2011
【分类号】：P145.6
[Abstract]:This paper deals with the author's research work in the master stage, including the investigation of the observation progress of short-time scale temporary radio phenomena and the study of the geometric structure of the pulsar PSR B1259-63. The main research work is to determine the calculation of the pulsar's magnetic dip angle 伪 and the angle 尾 between the direction of sight and the magnetic axis. These two parameters are important physical quantities to characterize the characteristics of the pulsar's radiating cone, and cannot be directly given by observation. It can only be obtained from the geometric study and statistical analysis of the polar crown model. The determination of these two parameters is of great significance to the establishment of magnetosphere structure and radiation mechanism of pulsars. In the second chapter of this paper, the recent research progress in the observation of short-time scale temporary radio is introduced. The short-time temporary radio source (RRATs) is a special radio source, compared with the ordinary pulsar. It has the following characteristics: it emits a few milliseconds of targeted explosive radio pulses, and the pulse has no periodicity during the emission period, that is, only one single radio pulse is transmitted at a time, so it is very difficult to detect this kind of radio source. At present, about 46 short-time temporary radio sources of this type have been found, of which about 27 have determined that they have a rotation period of second order, and 7 sources have measured periodic derivatives. In this chapter, some properties of these seven short-time scale temporary radio sources with measured periodic derivatives and their relationship with other known neutron stars are introduced. In the third chapter, the geometrical structure of PSR B 1259-63 polar crowns is studied. In this chapter, the possible polar crown geometry of the pulsar is studied by using the linear polarization position angle data of PSR B1259-63 at 1.52GHz 4.68GHz and 8.28GHz in the (EPN) database of the European Pulsar Observatory. In this study, we assume that PSR B1259-63 is a parallel rotor and a vertical rotor, and use the pulsar rotation vector model (RVM) to fit the linear polarization angle data by least square method. Under the assumption of parallel rotors, two sets of possible model parameters (AGB) were obtained by fitting the three frequency observations. The model (a) 伪 = 10.0 卤0.5 0, 尾 = 0.5 0 卤0.3 0, model (b) 伪 = 36.33 卤2 0, 尾 = 9 0 卤2.0, respectively, and a = 0 0 卤0 0, 尾 = 10 0 卤0 0, 尾 = 0 0 卤0 0, respectively, for model (b), 伪 = 36. 3 卤2. 0, 尾 = 9. 0 卤2. 0, respectively. This is basically consistent with the results obtained by Manchester and Johnston in 1995. On the assumption of vertical rotor, the main pulse (MP) and intermediate pulse (IP) data of three frequencies were fitted to obtain two magnetic pole parameters: 伪 MP=83~0 卤2 0, 尾 MP=-3~0 卤1 0 and 伪 IP=97~0 卤1 0, 尾 IP=-17~0 卤1 0, respectively, and the two magnetic pole parameters are 伪 MP=83~0 卤2 0, 尾 MP=-3~0 卤1 0 and 伪 IP=97~0 卤1 0, 尾 IP=-17~0 卤1 0, respectively. It is shown that the main pulse and the intermediate pulse may originate from the two poles of the pulsar respectively, and the possibility that the star is a vertical rotor can not be ruled out. The current observational data cannot clearly define the polar crown geometry of PSR B1259-63, so it is necessary to make further observation and study. In the fourth chapter, the work of this paper is summarized.
【学位授予单位】：新疆大学
【学位级别】：硕士
【学位授予年份】：2011
【分类号】：P145.6
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