一种脉冲星信号模拟新方法

贝晓敏; 帅平; 黄良伟; 孙海峰; 吴耀军; 张倩

doi:10.7498/aps.63.219701

摘要

在脉冲星导航地面实验中,为解决地面无法接收脉冲星辐射的X射线信号的问题,必须在实验系统中模拟脉冲星辐射信号. 本文提出两种全新脉冲星信号模拟方法. 第一种方法基于统计物理模型,该方法克服了常用泊松模型模拟方法中仿真适应性窄、仿真速度慢和时间分辨率低等不足,实现了对任意随机过程的脉冲信号进行快速高时间分辨率的仿真;第二种方法基于优化统计模型,该方法针对非齐次泊松过程信号的特性进行优化,仿真速度比常用泊松模型模拟方法提高至少30 倍,对于低流量脉冲星,甚至提高4个数量级,可实现纳秒级时间分辨率仿真.

关键词:

Abstract

Since X-ray pulsar signals cannot be detected on the ground, the pulsar signals need be simulated using the ground experiments. In this paper,two new simulation methods to obtain the time of arrival are put forward. The first method is based on a statistical physics model, which should overcome the shortcomings of narrow adaptation, low speed, and low time resolution in normal simulation method. This method has a high time-resolution and rapid simulation for any random pulse signals. 23 Another one is for the optimization of statistical models that satisfy signals in non-homogeneous Poisson process. The is second method has an improved simulation speed at least 30 times higher than the common Poisson model, even achieves four orders of magnitude greater than that for low flow pulsars, and this method also achieves a nanosecond time resolution simulation.

Keywords:

作者及机构信息

1.
钱学森空间技术实验室, 北京 100094;

2.
西安电子科技大学电子工程学院, 西安 710071

Authors and contacts

1.
Qian Xuesen Laboratory of Space Technology, Beijing 100094, China;

2.
School of Electronic Engineering, Xidian University, Xi'an 710071, China

参考文献

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施引文献

[1]	Shuai P, Li M, Chen S L, Huang Z 2009 Principles and Techniquesof X-ray Pulsar-Based Navigation System (Beijing: China Astronauic Publishing House) p14 (in Chinese) [帅平, 李明, 陈绍龙, 黄震 2009 X射线脉冲星导航系统原理与方法 (北京: 中国宇航出版社) 第14页]
[2]	Hanson J E 1996 Ph. D. Dissertation (Stanford: Stanford University)
[3]
[4]	Sheikh S I 2005 Ph. D. Dissertation (Maryland: University of Mary-land)
[5]
[6]	Emadzadeh A A, Speyer J L 2011 Navigation in space by X-ray pulsars (Berlin: Springer)
[7]
[8]
[9]	Sala J, Urruela A, Villares X 2004 ARIADNA Study 03 4202
[10]
[11]	Bernhardt M G, Prinz T, Becker W 2010 In: Proc of High Time Resolution Astrophysics IV, PoS (HTRA-IV) 050, Agios Nikolaos, Crete, Greece, 2010: 1-5
[12]
[13]
[14]	Bernhardt M G, Becker W, Prinz T, 2011 In: IEEE Proc of 2nd International Conference on Space Technology Athens, Greece, 2011: 1-4
[15]
[16]	Becker W 2009 X-ray emission from pulsars and neutron stars, in neutron stars and pulsars (Berlin: Springer, 2009: 91-140)
[17]	Zhu J, Ji P Y 2008 Chin. Phys. B 17 356
[18]
[19]
[20]	Zhang L, Bian X, Mei D C 2001 Chin. Phys. 10 662
[21]
[22]	Xu C X, He H L, He H H, Chen Y Z, Li H D, Jiang Y L 1999 Chin. Phys. 8 63
[23]	Zhao M, Huang T Y 2009 Science in China (G) 39 1671 (in Chinese) [赵铭, 黄天衣 2009 中国科学: 物理学力学天文学 39 1671]
[24]
[25]	Fei B J, Sun W J, Pan G T, Ji C X 2010 Chin. J. Space. Sci. 30 85 (in Chinese) [费保俊, 孙维瑾, 潘高田, 季诚响 2010 空间科学学报 30 85]
[26]
[27]	Li J X, Ke X Z 2009 Sci. Sin. G: Pysica, Mechanica Astronomica 39 311 (in Chinese) [李建勋, 柯熙政 2009 中国科学G辑: 物理学, 力学, 天文学 39 311]
[28]
[29]
[30]	Huang L W, Liang B, Zhang T, et al. 2012 Science in China Series G: Physics, Mechanics Astronomy 55 527
[31]	Sun S M, Zheng W, Tang G J, Li M 2009 Acta Astron. Sin. 50 325 (inChinese) [孙守明, 郑伟, 汤国建, 李满 2009 天文学报 50 325]
[32]
[33]	Mao Y 2009 Ph. D. Dissertation (Zhengzhou: PLA Information Engi-neering University) (in Chinese) [毛悦 2009 博士学位论文 (郑州: 解放军信息工程大学)
[34]
[35]
[36]	Zhou Q Y, Ji J F, Wang T 2013 Acta Phys. Sin. 62 019701 (in Chinese) [周庆勇, 姬剑锋, 任红飞 2013 62 019701]
[37]
[38]	Huang L W, Liang B, Zhang T 2013 Science in China Series G: Physics, Mechanics Astronomy 56 848
[39]
[40]	Huang L W, Liang B, Zhang T 2013 Science in China Series G: Physics, Mechanics Astronomy 56 848
[41]	Wang W B, Zhang X D, Wang X L 2013 Acta Phys. Sin. 62 069701 (in Chinese) [王文波, 张晓东, 汪祥莉 2013 62 069701]
[42]
[43]
[44]	Wang L, Xu L P, Zhang H, Luo N 2013 Acta Phys. Sin. 62 139702 (in Chinese) [王璐, 许录平, 张华, 罗楠 2013 62 139702]
[45]
[46]	Wang W B, Wang X L 2013 Acta Phys. Sin. 62 209701 (in Chinese) [王文波, 汪祥莉 2013 62 209701]
[47]
[48]	Hu H J, Zhao B S, Sheng L Z, Sai X F, Yan Q R, Chen B M, Wang P 2012 Acta Phys. Sin. 61 019701 (in Chinese) [胡慧君, 赵宝升, 盛立志, 赛小锋, 鄢秋荣, 陈宝梅, 王朋 2012 61 019701]
[49]	Su Z, Xu L P, Wang T 2011 Acta Phys. Sin. 60 119701 (in Chinese) [苏哲, 许录平, 王婷 2011 60 119701]
[50]
[51]
[52]	Hu H J, Zhao B S, Sheng L Z, Yan Q R 2011 Acta Phys. Sin. 60 029701 (in Chinese) [胡慧君, 赵宝升, 盛立志, 鄢秋荣 2011 60 029701]
[53]	Sun H F, Xie K, Li X P, Fang H Y, Liu X P, Fu L Z, Sun H J, Xue M F 2013 Acta Phys. Sin. 62 109701 (in Chinese) [孙海峰, 谢楷, 李小平, 方海燕, 刘秀平, 傅灵忠, 孙海建, 薛梦凡 2013 62 109701]
[54]
[55]	Sheng L Z, Zhao B S, Wu J J, Zhou F, Song J, Liu Y A, Shen J S, Yan Q R, Deng N Q, Hu H J 2013 Acta Phys. Sin. 62 129702 (in Chinese) [盛立志, 赵宝升, 吴建军, 周峰, 宋娟, 刘永安, 申景诗, 鄢秋荣, 邓宁勤, 胡慧君 2013 62 129702]
[56]
[57]	ZhengW, Sun S M, Tang G J 2010 1st China Satellite Navigation Con-ference Beijing China, May 18-22, 2010 (in Chinese) [郑伟, 孙守明, 汤国建 2010 第一届中国卫星导航学术年会北京 2010 5月 1822]
[58]
[59]	Emadzadeh A A, Speyer J L 2010 IEEE Trans. Sig. Proc. 58 4484
[60]
[61]
[62]	Landau L D, Lifshitz E M 1968 Statistical Physics (Part 1) (New York: Pergamon)
[63]	Du Y J, Qiao G J, Han J L, Wang W 2012 ApJ 84 748,
[64]

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