本文選題：脈沖星　切入點(diǎn)：雙星系統(tǒng)　出處：《華中科技大學(xué)》2016年碩士論文　論文類型：學(xué)位論文

【摘要】：脈沖星高速旋轉(zhuǎn)的中子星,其極端的物理?xiàng)l件如高密度、高溫度、高磁場、高速旋轉(zhuǎn)等可以幫助我們了解致密星體的物理構(gòu)成。脈沖雙星系統(tǒng)的精確的到達(dá)時(shí)間測量,可以使我們檢驗(yàn)廣義相對論和其它引力理論給出的不同預(yù)言。本論文圍繞脈沖雙星系統(tǒng)中脈沖星制動指數(shù)的異常展開。觀測數(shù)據(jù)顯示了脈沖雙星系統(tǒng)的制動指數(shù)遠(yuǎn)大于單個(gè)脈沖星的指制動數(shù)。我們認(rèn)為脈沖雙星系統(tǒng)中多普勒殘余引起的時(shí)間殘差可以影響脈沖雙星的頻率一階導(dǎo)數(shù)和二階導(dǎo)數(shù)從而使得脈沖雙星的制動指數(shù)遠(yuǎn)大于3。該研究在脈沖星的理論和應(yīng)用研究方面具有重要意義。理解脈沖星的自轉(zhuǎn)減慢機(jī)制,可以使我們更加了解脈沖星到達(dá)時(shí)間殘差的起因。從而為利用脈沖星到達(dá)時(shí)間檢驗(yàn)廣義相對論性預(yù)言的引力波、以及脈沖星導(dǎo)航等創(chuàng)造更加好的條件。論文分為六章。第一章綜述了脈沖星及研究的基本問題,內(nèi)容包括脈沖星的內(nèi)部結(jié)構(gòu),物態(tài)方程,質(zhì)量半徑關(guān)系。介紹了典型的脈沖星輻射區(qū)。第二章對脈沖星制動指數(shù)進(jìn)行介紹,對脈沖星的能量來源,自轉(zhuǎn)減慢進(jìn)行探討。按經(jīng)典的磁偶極輻射模型,脈沖星的制動指數(shù)應(yīng)該等于3。然而根據(jù)脈沖雙星的自轉(zhuǎn)頻率和自轉(zhuǎn)頻率的一階導(dǎo)數(shù)和二階導(dǎo)數(shù),得出的制動指數(shù)往往遠(yuǎn)大于3。第三章介紹脈沖雙星系統(tǒng)到達(dá)時(shí)間測量模型,對脈沖星到達(dá)時(shí)間處理軟件Tempo2進(jìn)行介紹。觀測者接收到的脈沖星信號往往存在時(shí)間殘差。第四章研究21顆脈沖雙星系統(tǒng)的制動指數(shù)。通過引入脈沖星在軌道運(yùn)動中的多普勒殘余效應(yīng)對自轉(zhuǎn)頻率一階導(dǎo)數(shù)的貢獻(xiàn),使得自轉(zhuǎn)頻率的一階導(dǎo)數(shù)減小,進(jìn)而使得這些脈沖雙星的制動指數(shù)大幅度減小。結(jié)果21顆脈沖雙星中的絕大部分脈沖星的制動指數(shù)從十的四、五次方等降到了3左右。并結(jié)合軌道-自旋耦合模型和伴星引起的測地進(jìn)動軌道進(jìn)動模型,對剩余的修正后的脈沖星制動指數(shù)進(jìn)一步分析。第五章是將多普勒殘余效應(yīng)移植到脈沖雙星到達(dá)時(shí)間處理軟件Tempo2。在多普勒效應(yīng)引起的自轉(zhuǎn)頻率一階導(dǎo)數(shù)的變化導(dǎo)致的時(shí)間殘差不被忽略的情況下,所得到的時(shí)間殘差和不考慮脈沖雙星系統(tǒng)中多普勒殘余效應(yīng)得到的時(shí)間殘差進(jìn)行比較,在兩顆脈沖星的到達(dá)時(shí)間殘差降低或者不變的情況下,使脈沖星制動指數(shù)降到正常值。第六章是總結(jié)和展望。此部分總結(jié)了脈沖雙星系統(tǒng)中多普勒殘余效應(yīng)對脈沖雙星到達(dá)時(shí)間的影響,解釋了21顆脈沖雙星制動指數(shù)異常的問題。并對兩顆有到達(dá)時(shí)間觀測數(shù)據(jù)的脈沖雙星在Tempo2里實(shí)現(xiàn)了使制動指數(shù)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.
【學(xué)位授予單位】：華中科技大學(xué)
【學(xué)位級別】：碩士
【學(xué)位授予年份】：2016
【分類號】：P145.6

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