脉冲星磁层中带电粒子能损机制的研究
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摘要
脉冲星是中等质量的恒星演化到晚期经过超新星爆发后遗留下的致密天体.它具有很强的磁场,并快速旋转,且周期稳定,正因为此我们能接收到它所发出的周期性脉冲信号。本文关注的是脉冲星磁层中带电粒子的能损机制,主要探讨了带电粒子同步辐射过程中投射角随时间的演化关系及其应用,分析了共振逆康普顿散射机制对粒子能谱的影响。本论文的主要内容如下:
第一章简单介绍了脉冲星的研究历史,当今脉冲星研究的前沿课题,以及本课题的意义。第二章综述了射电脉冲星的观测特征,相关参量及射电辐射的经验模型和理论模型,其中以极冠区加速模型为重点。第三章依据相对论性电子速度分解,电子随动坐标系和实验室参照系的速度变换,导出并计算了同步辐射能损引起的电子投射角随电子运动路程的演化,并以此为基础计算了洛仑兹因子、同步辐射功率和特征频率的演化。结果表明在较强磁场条件下投射角通常迅速衰减,趋向于零,由此导致同步辐射功率远低于投射角恒定假设下的同步辐射功率。由于同步辐射对强磁场下极端相对论电子更为有效,因此会导致内、外加速区出射粒子流能谱分布的差异。典型的脉冲星表面温度为～10~5K,共振逆康普顿散射被证明是强磁场下次级粒子能损的主要机制。第四章以极冠区加速模型为基础,从理论上计算了次级粒子外流过程中,共振逆康普顿散射所造成的粒子能谱随高度的演化。我们修正了Lyubarskii和Petrova(LP00)在2000年同类工作中的计算错误,结果肯定了粒子能谱分布通常将变为高能和低能两个峰,粒子主要集中于低能段,但低能段电子数比重远高于LP00的结果。除了计算了Arons型初始能谱分布的演化,我们还计算了基于曲率光子引发级联过程所产生的一种简化次级粒子能谱,演化的最终能谱分布也表现为双峰形式。
Pulsars are compact objects formed from supernova outburst when moderately massive stars evole to their end. Due to the strong magnetic field and fast rotation of pulsars, we can receive their periodical pulse signals. The radiation of pulsars covers full band. This thesis focuses on energy loss of charged particles in pulsar magnetosphere. We mainly studied the evolution of particle pitch angle in synchrotron emission process and the application in pulsar emission, and the evolution of particle energy distribution caused by resonant inverse Compton scattering (RICS).
The research history of pulsars, the frontier and the motivation of this research are introduced in chapter 1. In chapter 2, we review the observation features, the present empirical models and theoretical models, among which the polar gap model is of perticular interest. In chapter 3, according to lorentz transform of comoving and laboratory reference frames, the evolution of pitch angle in synchrotron emission process is derived and calculated. The evolution of Lorentz factor, the emission power and the critical frequency are calculated also. It is shown that the pitich angle usually decreases rapidaly and results in much lower emission power than that under the assumption of constant pitch angle. Because synchrotron emissio is more efficient for relativistic particles in strong magnetic field, the energy distribution of secondary particles will be different in the cases of inner gap and outer gap.
In chapter 4, we calculated the evolution of energy distribution of secondary particles caused by the RICS under the frame of inner gap. The calculation error in the similar work done by Lyubarskii and Petrova (2000) is corrected. The results confirm that the secondary particles will concentrate on two Lorentz-factor peaks, one at low energy, and the other at high energy. However, the low energy bulge is sharper and contains more particles with respect to LP00's result. We also derive a new distribution based on the curvature radiation induced secondary particle distribution. The results also show the final distribution is double peaked.
第一章简单介绍了脉冲星的研究历史,当今脉冲星研究的前沿课题,以及本课题的意义。第二章综述了射电脉冲星的观测特征,相关参量及射电辐射的经验模型和理论模型,其中以极冠区加速模型为重点。第三章依据相对论性电子速度分解,电子随动坐标系和实验室参照系的速度变换,导出并计算了同步辐射能损引起的电子投射角随电子运动路程的演化,并以此为基础计算了洛仑兹因子、同步辐射功率和特征频率的演化。结果表明在较强磁场条件下投射角通常迅速衰减,趋向于零,由此导致同步辐射功率远低于投射角恒定假设下的同步辐射功率。由于同步辐射对强磁场下极端相对论电子更为有效,因此会导致内、外加速区出射粒子流能谱分布的差异。典型的脉冲星表面温度为～10~5K,共振逆康普顿散射被证明是强磁场下次级粒子能损的主要机制。第四章以极冠区加速模型为基础,从理论上计算了次级粒子外流过程中,共振逆康普顿散射所造成的粒子能谱随高度的演化。我们修正了Lyubarskii和Petrova(LP00)在2000年同类工作中的计算错误,结果肯定了粒子能谱分布通常将变为高能和低能两个峰,粒子主要集中于低能段,但低能段电子数比重远高于LP00的结果。除了计算了Arons型初始能谱分布的演化,我们还计算了基于曲率光子引发级联过程所产生的一种简化次级粒子能谱,演化的最终能谱分布也表现为双峰形式。
Pulsars are compact objects formed from supernova outburst when moderately massive stars evole to their end. Due to the strong magnetic field and fast rotation of pulsars, we can receive their periodical pulse signals. The radiation of pulsars covers full band. This thesis focuses on energy loss of charged particles in pulsar magnetosphere. We mainly studied the evolution of particle pitch angle in synchrotron emission process and the application in pulsar emission, and the evolution of particle energy distribution caused by resonant inverse Compton scattering (RICS).
The research history of pulsars, the frontier and the motivation of this research are introduced in chapter 1. In chapter 2, we review the observation features, the present empirical models and theoretical models, among which the polar gap model is of perticular interest. In chapter 3, according to lorentz transform of comoving and laboratory reference frames, the evolution of pitch angle in synchrotron emission process is derived and calculated. The evolution of Lorentz factor, the emission power and the critical frequency are calculated also. It is shown that the pitich angle usually decreases rapidaly and results in much lower emission power than that under the assumption of constant pitch angle. Because synchrotron emissio is more efficient for relativistic particles in strong magnetic field, the energy distribution of secondary particles will be different in the cases of inner gap and outer gap.
In chapter 4, we calculated the evolution of energy distribution of secondary particles caused by the RICS under the frame of inner gap. The calculation error in the similar work done by Lyubarskii and Petrova (2000) is corrected. The results confirm that the secondary particles will concentrate on two Lorentz-factor peaks, one at low energy, and the other at high energy. However, the low energy bulge is sharper and contains more particles with respect to LP00's result. We also derive a new distribution based on the curvature radiation induced secondary particle distribution. The results also show the final distribution is double peaked.
引文
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[52]Stairs,I.H.;Lyne,A.G.;Shemar,S.L.,Evidence for free precession in a pulsar,2000,Natur,406,484
[53]D.R.,Lorimer,Binary and Millisecond Pulsars at the New Millennium,2001,Living Reviews in Relativity
[54]Sieber W.,Reviwing pulsar spectra,2002,Physikzentrum Bad Honnef,Germany,Jan.21-25,
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[2] http://www.atnf.csiro.au/research/pulsar/psrcat/
[3] Ruderman,M.A & Sutherland,P.G., 1975, ApJ,196,51
[4] Hulse, R. A, Taylor, J. H.Discovery of a pulsar in a binary system 1975,ApJ...195L..51H
[5] Backer, D. C; Kulkarni, S. R.; Heiles, C; Davis, M. M.; Goss, W. M.A millisecond pulsar 1982Natur.300..615B
[6] Lyne, A. G.; Brinklow, A.; Middleditch, J.; Kulkarni, S. R.; Backer, D. C. The discovery of a millisecond pulsar in the globular cluster M28 1987Natur.328..399L
[7] Wolszczan, A.; Frail, D. A.A planetary system around the millisecond pulsar PSR1257+12 1992Natur.355..145W
[8] Backer, D. C; Foster, R. S.; Sallmen, S.A Second Companion of the Millisecond Pulsar 1620-26 1993Natur.365..817B
[9]Burgay, M.; D'Amico, N. An increased estimate of the merger rate of double neutron stars from observations of a highly relativistic system 2003Natur.426..531B
[10] Goldreich,P. & Julian W.,1969,APJ,157,869
[11] Ruderman,M.A & Sutherland,P.G., 1975, ApJ,196,51
[12] Wang D, Wu X J & Cheng H. A possible mechanisms for core emission from radio pulsars [J]. Vistas in Astron. 1988,31
[13]Muslimov, Alex G.; Harding, Alice K.Extended Acceleration in Slot Gaps and Pulsar High-Energy Emission 2003ApJ...588..430M
[14] G. J. Qiao, J. F. Liu, B. Zhang et al. An inverse Compton scattering (ICS) model of pulsar emission II [J]. 2001, A&A 377,964.
[15]Xu,R.X.,Strange Quark Stars - A Review,2003,in:High Energy Processes,Phenomena in Astrophysics,Proceedings of IAU Symposium No.214,eds.X.D.Li,Z.R.Wang V.Trimble,p.191-198
[16]Holloway,N.J.Pulsars-p-n junctions in pulsar magnetospheres 1973Natur.246....6H
[17]Zhang,Bing;Harding,Alice K,High Magnetic Field Pulsars and Magnetars:A Unified Picture,2000ApJ...535L..51Z
[18]Lyubarskii,Y.E.;Petrova,S.A.Resonant inverse Compton scattering by secondary pulsar plasma,2000AA...355..406L
[19]Sturrock,P,A On the Possibility of Pulsar Action in Quasars 1971,APJ,554,316
[20]Mulimov A.G,Harding,A K.,Particle Acceleration in High Field Pulsars and Magnetars 2002,astrp-ph/0301023
[21]Cheng,K,S,Ho,C.Ruderman,M,A.A Crab pulsar model-X-ray,optical,and radio emission 1977,APJ,515,337
[22]Melrose Gedalin 1999,Relativistic Plasma Emission and Pulsar Radio Emission:A Critique 1999ApJ...521..351M
[23]R,S,Buschauer,Benford,General theory of coherent curvature radiation 1976MNRAS.177..109B
[24]Ruderman,M.A & Sutherland,P.G.,1975,ApJ,196,51
[25]Gil,J.A.;Sendyk,M.Spark Model for Pulsar Radiation Modulation Patterns.2000ApJ...541..351G
[26]Melrose Gedalin 1999,Relativistic Plasma Emission and Pulsar Radio Emission:A Critique 1999ApJ...521..351
[27]Qiao,G.J.The Observational Phenomena of Quasiperiodie Oscillation in Low Mass X-Ray Binaries,1990PrA.....8...34Q
[28]Xu,R.X.,Strange Quark Stars - A Review,2003,in:High Energy Processes,Phenomena in Astrophysics,Proceedings of IAU Symposium No.214,eds.X.D.Li,Z.R.Wang V.Trimble,p.191-198
[29]Fritz,G.Henry,R.C.Meekins,J.F.Chubb,T.A.Friedman,H.X-ray Pulsar in the Crab Nebula 1969Scince 164..709F
[30]Kniffen,D.A.;Hartman,R.C.;Thompson,D.J.;Bignami,G.K.;Fichtel,C.E.;Turner,T.;Ogelman,H,Gamma radiation from the Crab Nebula above 35 MeV 1974Natur.251..397K
[31]Kniffen,D..SAS-2 high energy gamma-ray observations of galactic structure and the Crab nebula.1975sast.nasa...52K
[32]Pavlov,G.G.;Zavlin,V.E.;Sanwal,D.Thermal Radiation from Neutron Stars:Chandra Results.2002nsps.conf..2.73P
[33]李启斌,李宗伟等,90年代天体物理学,1996,高等教育出版社,200-202。
[34]Weisberg,J.M.;Romani,R.W.;Taylor,J.H.Evidence for geodetic spin precession in the binary pulsar 1913 + 16.1989ApJ...347.1030W
[35]Lyric,A.G.;Stairs,I.H.;Shemar,S.L.Periodicities in Rotation and Pulse Shape in PSR B1828-11.2000ASPC..202...93L
[36]Staelin,D.H.;Reifenstein,E.C.Pulsating radio sources near the Crab Neb-1968Sci...162.1481S
[37]Cognard,I.;Shrauner,J.A.;Taylor,J.H.;Thorsett,S.E.Giant Radio Pulses from a Millisecond Pulsar.1996ApJ...457L..81C
[38]Goldman,Martin V.Strong turbulence of plasma waves.1984RvMP...56..709G
[39]Maron O.,Kijak J.et al.,Pulsar spectra of radio emission A&A,2000,
[40]Malofeev V.,Gil J.et al.,Spectra of 45pulsars,1994,A&A,285,201 - 208,
[41]Kijak J.,Gupta Y.,& Krzeszowski K.,Turn-over in pulsar spectra around 1GHz,April 8,2007,
[42]Goldreich,P.& Julian W.;1969,APJ,157,869
[43]Thorsett,Stephen.ErikObserving millisecond and binary.pulula.sars.1991PhDT.........2T
[45]Gil J.A.Sendyk M.,Spark Model for Pulsar Radiation Modulation Patterns,ApJ,2000,541,351
[46]Cheng,K.S.,Ho,C.Ruderman,M.A.,Energetic Radiation from Rapidly Spinning Pulsars.Ⅱ.,ApJ,1986a,300,500
[47]Cheng,K.S.,Ho,C.Ruderman,M.A.,Energetic radiation from rapidly spinning pulsars.Ⅰ.,ApJ,1986b,300,522
[48]Cheng K S,Ruderman M A,Zhang L.,A Three-dimensional Outer Magnetospheric Gap Model for Gamma-Ray Pulsars,ApJ,2000,537:964
[49]Hirotani,K.,Shibata,S.,One-dimensional electric field structure of an outer gap accelerator-Ⅱ,MNRAS,1999,308,67
[50]Takata J.,Shibata S.,Hirotani K.,Chang,H.-K.,A two-dimensional electrody-namical outer gap model for γ-ray pulsars:γ-ray spectrum,MNRAS,2006,366,1310
[51]G.J.Qiao,K.J.Lee,H.G.Wang,R.X.Xu and J.L.Han,The annular gap for pulsar radiation:γ-ray and radio emission,ApJ,2004,606:L49-L52,
[52]Stairs,I.H.;Lyne,A.G.;Shemar,S.L.,Evidence for free precession in a pulsar,2000,Natur,406,484
[53]D.R.,Lorimer,Binary and Millisecond Pulsars at the New Millennium,2001,Living Reviews in Relativity
[54]Sieber W.,Reviwing pulsar spectra,2002,Physikzentrum Bad Honnef,Germany,Jan.21-25,
[55]Komesaroff M.,Possible Mechanism for the Pulsar Radio Emission,14 February 1970,Nature 225,612-614
[56]Backer D.,Pulsar average wave forms and hollow-cone beam models,11/1976,ApJ,209,895-907
[57]Rankin J.M.,Toward an empirical theory of pulsar emission I.ApJ,1983b,274,359
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