【摘要】：本文內(nèi)容涉及作者在碩士生階段的研究工作,包括對(duì)短時(shí)標(biāo)暫現(xiàn)射電現(xiàn)象觀測(cè)研究進(jìn)展的探討和對(duì)脈沖星PSR B1259-63極冠幾何結(jié)構(gòu)的研究。主要研究工作是在確定脈沖星磁傾角α以及視線方向與磁軸之間的夾角β的計(jì)算上,這兩個(gè)參量是表征脈沖星輻射錐特性的重要物理量,不能由觀測(cè)直接給出,只能由極冠模型的幾何研究和統(tǒng)計(jì)分析來獲得。這兩個(gè)參量值的確定對(duì)脈沖星的磁層結(jié)構(gòu)和輻射機(jī)制的確立都有重要意義。 本文第二章介紹了目前國(guó)內(nèi)外對(duì)短時(shí)標(biāo)暫現(xiàn)射電現(xiàn)象觀測(cè)研究進(jìn)展方面的討論,短時(shí)標(biāo)暫現(xiàn)射電源(RRATs)是一類特殊的射電源,與普通脈沖星相比,它具有以下的特征:發(fā)射稀少的毫秒級(jí)時(shí)標(biāo)的爆發(fā)式射電脈沖,發(fā)射期內(nèi)脈沖沒有周期性,即每次只發(fā)射一個(gè)單獨(dú)的射電脈沖,所以探測(cè)這類射電源非常困難。目前共發(fā)現(xiàn)大約46個(gè)這種類型的短時(shí)標(biāo)暫現(xiàn)射電源,其中大約27個(gè)已確定了它們有秒級(jí)自轉(zhuǎn)周期,7個(gè)源測(cè)得了周期導(dǎo)數(shù)。本章主要介紹這7個(gè)已測(cè)得周期導(dǎo)數(shù)的短時(shí)標(biāo)暫現(xiàn)射電源的一些性質(zhì)及它們與其它已知的幾類中子星的關(guān)系與區(qū)別。 本文第三章介紹了對(duì)脈沖星PSR B1259-63極冠幾何結(jié)構(gòu)的研究。本章利用歐洲脈沖星觀測(cè)網(wǎng)(EPN)數(shù)據(jù)庫(kù)里PSR B1259-63在1.52GHz、4.68GHz和8.28GHz三個(gè)頻率上的線偏振位置角觀測(cè)數(shù)據(jù)研究這顆脈沖星可能的極冠幾何結(jié)構(gòu)。本研究分別假設(shè)了PSR B1259-63是平行轉(zhuǎn)子和垂直轉(zhuǎn)子兩種情況,用脈沖星旋轉(zhuǎn)矢量模型(RVM)對(duì)線偏振位置角觀測(cè)數(shù)據(jù)進(jìn)行了最小二乘法擬合研究。在平行轉(zhuǎn)子假設(shè)下,對(duì)三個(gè)頻率觀測(cè)結(jié)果擬合得到了兩套可能的模型(a、b)參數(shù),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,這與Manchester和Johnston在1995年得到的結(jié)果基本一致。在垂直轉(zhuǎn)子假設(shè)下,對(duì)三個(gè)頻率觀測(cè)的主脈沖(MP)和中間脈沖(IP)數(shù)據(jù)擬合得到兩個(gè)磁極參數(shù)分別為αMP=83~0±2~0、βMP=-3~0±1~0和αIP=97~0±1~0、βIP=-17~0±1~0,表明主脈沖和中間脈沖可能分別源自脈沖星兩個(gè)磁極,不能排除該星是垂直轉(zhuǎn)子的可能性。目前的觀測(cè)數(shù)據(jù)還不能明確限定PSR B1259-63的極冠幾何結(jié)構(gòu),有必要進(jìn)行更深入的觀測(cè)與研究。 在第四章里總結(jié)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 偽 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) 偽 = 10.0 鹵0.5 0, 尾 = 0.5 0 鹵0.3 0, model (b) 偽 = 36.33 鹵2 0, 尾 = 9 0 鹵2.0, respectively, and a = 0 0 鹵0 0, 尾 = 10 0 鹵0 0, 尾 = 0 0 鹵0 0, respectively, for model (b), 偽 = 36. 3 鹵2. 0, 尾 = 9. 0 鹵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: 偽 MP=83~0 鹵2 0, 尾 MP=-3~0 鹵1 0 and 偽 IP=97~0 鹵1 0, 尾 IP=-17~0 鹵1 0, respectively, and the two magnetic pole parameters are 偽 MP=83~0 鹵2 0, 尾 MP=-3~0 鹵1 0 and 偽 IP=97~0 鹵1 0, 尾 IP=-17~0 鹵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.
【學(xué)位授予單位】：新疆大學(xué)
【學(xué)位級(jí)別】：碩士
【學(xué)位授予年份】：2011
【分類號(hào)】：P145.6

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