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X射线脉冲轮廓稳定性对导航精度的影响

孙海峰 包为民 方海燕 李小平

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X射线脉冲轮廓稳定性对导航精度的影响

孙海峰, 包为民, 方海燕, 李小平

Effect of stability of X-ray pulsar profiles on range measurement accuracy in X-ray pulsar navigation

Sun Hai-Feng, Bao Wei-Min, Fang Hai-Yan, Li Xiao-Ping
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  • X射线脉冲星具有广阔的导航应用前景,稳定的脉冲轮廓是自主导航的基础,然而在X射线脉冲轮廓的稳定性及其对导航精度的影响方面一直缺乏系统的研究. 采用Pearson相关系数、标准偏差及功率谱熵三组指标量化脉冲轮廓的稳定性. 利用罗西X射线计时探测器卫星X射线段(2–16 keV)11 年的观测资料,统计了包括周期跃变在内的Crab脉冲轮廓稳定性. 在此基础上,引入Cramer-Rao理论建立了脉冲轮廓稳定性对距离测量误差影响的数学模型,并通过分析各误差因素确定脉冲轮廓稳定性对距离测量误差的影响范围. 实测数据处理表明,Crab脉冲星的X射线脉冲轮廓具有极高的稳定性,跃变期间脉冲轮廓无明显变化,脉冲轮廓的稳定性导致沿脉冲星方向上产生34 m±25 m的距离测量误差.
    The Crab pulsar is an isolated rotation-powered pulsar which emits large X-ray fluxes, making it a candidate source for carrying out the X-ray pulsar navigation (XNAV). The long-term stable profiles are considered as the foundation of XNAV. However, systematic studies of the long-term stability of the X-ray pulsar profile and its effect on range accuracy in XNAV are lacking. In this paper, we use the X-ray band (2–16 keV) data monitored by Rossi X-ray timing explorer (RXTE) spacecraft over the latest 11 years, to first investigate the stability of the Crab pulsar including the profiles after the glitches. Furthermore, some measurements of the long-term profile shape, including Pearson correlation coefficient, standard deviation and spectral entropy, are presented both in the time domain and in the frequency domain. In the data processing, the Fourier analysis and cross-correlation are used to deal with the 191 RXTE data sets. With the help of the Cramer-Rao theory, the effect of the profile variation on the error of the range determination in XNAV is studied. Furthermore, after analyzing those errors, the effect of the stability of the Crab pulsar on range determination is confined to more narrow limits. The results demonstrate that the 2–16 keV profiles are almost constant during the period 2001–2012. The profiles after the glitches show no significant discrepancy. The variation of Crab profile inevitably has an influence on the navigation precision to a certain extent. The calculated range error along the pulsar line-of-sight due to the stability of the pulsar profile is 34 m±25 m.
    • 基金项目: 中央高等学校基金(批准号:K72125087)资助的课题.
    • Funds: Project supported by the Fundamental Scientific Research Foundation for the Central Universities of China (Grant No. K72125087).
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    Jain C, Paul B 2011 Res. Astron. Astrophys. 11 1134

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    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 物理学报 62 109701]

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    Ge M Y 2012 Ph. D. Dissertation (Beijing: Institute of High Energy Physics, Chinese Academy of Sciences) (in Chinese) [葛明玉 2012 博士学位论文 (北京: 中国科学院高能物理研究所)]

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    Espinoza C M, Lyne A G, Stappers B W, Kramer M 2011 Mon. Not. Roy. Astron. Soc. 414 1679

    [19]

    Sheikh S I 2005 Ph. D. Dissertation (College Park: University of Maryland)

    [20]

    Hui C Y, Cheng K S 2004 Astrophys. J. 608 935

    [21]

    Emadzadeh A A 2009 Ph. D. Dissertation (Los Angeles: University of California Los Angeles)

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    Taylor J H 1992 Philos. Trans. Roy. Soc. A 341 117

    [23]

    Xie Z H, Xu L P, Ni G R 2008 Acta Phys. Sin. 57 6683 (in Chinese) [谢振华, 许录平, 倪广仁 2008物理学报 57 6683]

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  • [1]

    Shuai P, Li M, Chen S L, Huang Z 2009 Principles and Techniques of X-ray Pulsar Based Navigation System (Beijing: China Astronautic Publishing House) p20 (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20页]

    [2]

    Emadzadeh A A, Speyer J L 2010 IEEE Trans. Signal Proces. 58 4484

    [3]

    Zhou Q Y, Ji J F, Ren H F 2013 Acta Phys. Sin. 62 139701 (in Chinese) [周庆勇, 姬剑锋, 任红飞 2013 物理学报 62 139701]

    [4]

    Hanson J, Sheikh S, Graven P, Collins J 2008 Proceeding IEEE/ION: Position, Location and Navigation Symposium Monterey, USA, May 5–8, 2008 p704

    [5]

    Zhu J, Ji P Y 2008 Chin. Phys. B 17 356

    [6]

    Zhang H, Xu L P 2011 Acta Phys. Sin. 60 039701 (in Chinese) [张华, 许录平 2011 物理学报 60 039701]

    [7]

    Pan J, Wu X J 1999 Chin. Phys. Lett. 16 307

    [8]

    Helfand D J, Manchester R N, Taylor J H 1975 Astrophys. J. 198 661

    [9]

    Rathnasree N, Rankin J M 1995 Astrophys. J. 452 814

    [10]

    Vivekanand M 2001 Astron. Astrophys. 373 236

    [11]

    Rots A H, Jahoda K, Lyne A G 2004 Astrophys. J. 605 L129

    [12]

    Molkov S, Jourdain E, Roques J P 2010 Astrophys. J. 708 403

    [13]

    Jain C, Paul B 2011 Res. Astron. Astrophys. 11 1134

    [14]

    Liu X P, Li X P, Sun H F 2013 Acta Opt. Sin. 33 0304002 (in Chinese) [刘秀平, 李小平, 孙海峰 2013 光学学报 33 0304002]

    [15]

    Kaiper L, Hermsen W, Walter R, Foschini L 2006 Astron. Astrophys. 411 L31

    [16]

    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 物理学报 62 109701]

    [17]

    Ge M Y 2012 Ph. D. Dissertation (Beijing: Institute of High Energy Physics, Chinese Academy of Sciences) (in Chinese) [葛明玉 2012 博士学位论文 (北京: 中国科学院高能物理研究所)]

    [18]

    Espinoza C M, Lyne A G, Stappers B W, Kramer M 2011 Mon. Not. Roy. Astron. Soc. 414 1679

    [19]

    Sheikh S I 2005 Ph. D. Dissertation (College Park: University of Maryland)

    [20]

    Hui C Y, Cheng K S 2004 Astrophys. J. 608 935

    [21]

    Emadzadeh A A 2009 Ph. D. Dissertation (Los Angeles: University of California Los Angeles)

    [22]

    Taylor J H 1992 Philos. Trans. Roy. Soc. A 341 117

    [23]

    Xie Z H, Xu L P, Ni G R 2008 Acta Phys. Sin. 57 6683 (in Chinese) [谢振华, 许录平, 倪广仁 2008物理学报 57 6683]

    [24]

    Li J X, Ke X Z, Zhao B S 2012 Acta Phys. Sin. 61 069701 (in Chinese) [李建勋, 柯熙政, 赵宝升 2012 物理学报 61 069701]

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出版历程
  • 收稿日期:  2013-08-21
  • 修回日期:  2013-11-21
  • 刊出日期:  2014-03-05

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