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The pulsar ephemeris that maintains the time-space benchmark for pulsar navigation is an important part of Xray pulsar navigation system. The parameters of pulsar timing model which are contained in the pulsar ephemeris can influence directly the accuracy of pulsar navigation. Some studies have shown that 100 m target of X-ray pulsar navigation should need 1 mas angle position and 100 ns pulse time of arrival, the high-level precision of parameters of some pulsars can be reached by ground radio observations with large-diameter telescope. Owing to the development of high-performance X-ray detector and stable space observation platform, the technology that the parameters of pulsar ephemeris are measured by space X-ray observations may be achieved, so the feasibility of this technology is studied in this paper by reconstructing the analysis process. The process includes mainly three parts. Firstly, the methods of simulating X-ray pulsar signals, replicating pulse profile and getting the time of arrival between the observed pulse profile and the standard one from analyzing observation data of the RXTE and Chandra satellite are studied, then the accuracies of X-ray space observations for four pulsars are estimated by using the large sample duplication events. Secondly, the process of fitting model for ephemeris parameters is established and realized by computer program in C++ language. Finally, the relationships between the accuracies of ephemeris parameters and those of the following factors are analyzed: the observation accuracy, the observation duration, the observed frequency. Those results of four pulsars (Crab, B1937+21, B1821-24 and B1509-58) are concluded below. 1) The X-ray space timing precisions of Crab pulsars in the observation durations of 1000 s and an hour are 1.41 s and 0.83 s respectively, the ones of other 3 pulsars in three different observation durations of 1000 s, an hour, and a day are also gained. 2) The ephemeris parameters of four pulsars are achieved by the X-ray space simulation observations, which are similar to the result of ground pulsar radio timing, the precision of right ascension is better than that of declination. 3) The precisions of ephemeris parameters can be improved by increasing the times of observation. 4) If each pulsar can be observed for 1000 s by space satellite every half an month with a 1 m2 effective area detector, the precisions of the estimated parameters (RA, DEC and Period) for Crab pulsar are 23.4 mas 806.0 mas, 8.121310-8 s, those of other three pulsars are gained and analyzed. However, owing to the low-flux radiation characteristics of millisecond X-ray pulsar and the demand for light and efficient large detector, the high-precision ephemeris parameters can be achieved difficultly by using the space X-ray observations, but can be established and maintained well by the ground radio observation technology. The suggestion for promoting the construction of some large-diameter telescopes is made, and the method that the behavior of X-ray emissions from pulsar is predicted by the ground radio observations still needs be studied.
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Keywords:
- pulsar navigation /
- timing model /
- pulsar timing
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[2] Sheikh S I 2005 Ph. D. Dissertation (Maryland: Department of Aerospace Engineering, University of Maryland)
[3] Sun H F, Bao W M, Fang H Y, Li X P 2014 Acta Phys. Sin. 63 069701 (in Chinese) [孙海峰, 包为民, 方海燕, 李小平 2014 63 069701]
[4] 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]
[5] Zhou Q Y, Ren H F 2013 Geomatics Science and Engineering 33 21 (in Chinese) [周庆勇, 任红飞 2013测绘科学与工程 33 21]
[6] Lorimer D R, Kramer M 2005 Handbook of Pulsar Astronomy (London: Cambridge University Press)
[7] Manchester R N 2013 Classical and Quantum Gravity 30 224010
[8] Deller A T 2009 Ph. D. Dissertation (Hawthorn: Faculty of Information and Communication Technology Swinburne University)
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[10] Zhang S N 2012 Sci. China G 42 1308 (in Chinese) [张双南 2012 中国科学: 物理学 力学 天文学 42 1308]
[11] Ge M Y 2012 Ph. D. Dissertation (Beijing: Chinese Academy of Sciences) (in Chinese) [葛明玉 2012 博士学位论文 (北京: 中国科学院研究生院)]
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[14] Emadzadeh A A, Speyer J 2011 Navigation in Space by X-ray Pulsars (London: Springer)
[15] Huang L W 2013 Ph. D. Dissertation (Beijing: Tsinghua University) (in Chinese) [黄良伟 2013 博士学位论文 (北京: 清华大学)]
[16] Taylor J H 1992 Phil. Trans. R. Soc. Lond. A 341 117
[17] Edwards R T, Hobbs G B, Manchester R N 2006 MNAS 372 1549
[18] Downs G S, Reichley P E 1983 Astrophys. J. (Supplement Series) 53 169
[19] Zhou Q Y, Ji J F, Ren H F 2014 Acta Phys. Sin. 62 139701 (in Chinese) [周庆勇, 姬剑锋, 任红飞 2013 62 139701]
[20] Scott D M, Finger H M, Wilson E A 2003 MNAS 344 412
[21] Dolch T, Lam M T, Cordes J, et al. 2014 Astrophys. J. 794 21
[22] Graven P, Collins J, Sheikh S I, et al. 2008 31st Annual AAS Guidance and Control Conference Breckenridge, Colorado, February 1-6, 2008 AAS 08-054
[23] Peng B, Jin C J, Du B, et al. 2012 Sci. China G 42 1292 (in Chinese) [彭勃, 金乘进, 杜彪, 等 2012 中国科学: 物理学 力学 天文学 42 1292]
[24] Nan R D 2005 Sci. China G 35 449 (in Chinese) [南仁东 2005 中国科学: 物理学 力学 天文学 35 449]
[25] Shen Z Q 2013 Science (KEXUE) 63 15 (in Chinese) [沈志强 2013 科学 63 15]
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[1] Zhou Q Y 2011 M. S. Dissertation (Zhengzhou: PLA Information Engineering University) (in Chinese) [周庆勇 2011硕士学位论文(郑州: 解放军信息工程大学)]
[2] Sheikh S I 2005 Ph. D. Dissertation (Maryland: Department of Aerospace Engineering, University of Maryland)
[3] Sun H F, Bao W M, Fang H Y, Li X P 2014 Acta Phys. Sin. 63 069701 (in Chinese) [孙海峰, 包为民, 方海燕, 李小平 2014 63 069701]
[4] 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]
[5] Zhou Q Y, Ren H F 2013 Geomatics Science and Engineering 33 21 (in Chinese) [周庆勇, 任红飞 2013测绘科学与工程 33 21]
[6] Lorimer D R, Kramer M 2005 Handbook of Pulsar Astronomy (London: Cambridge University Press)
[7] Manchester R N 2013 Classical and Quantum Gravity 30 224010
[8] Deller A T 2009 Ph. D. Dissertation (Hawthorn: Faculty of Information and Communication Technology Swinburne University)
[9] Wang N 2014 Sci. China G 44 783 (in Chinese) [王娜 2014 中国科学: 物理学 力学 天文学 44 783]
[10] Zhang S N 2012 Sci. China G 42 1308 (in Chinese) [张双南 2012 中国科学: 物理学 力学 天文学 42 1308]
[11] Ge M Y 2012 Ph. D. Dissertation (Beijing: Chinese Academy of Sciences) (in Chinese) [葛明玉 2012 博士学位论文 (北京: 中国科学院研究生院)]
[12] Livingstone M A, Kaspi V M, Gavriil F P 2005 Astrophys. J. 633 1095
[13] Xu C X, He H L, He H H, Chen Y Z, Li H D, Jiang Y L 1999 Acta Phys. Sin. (Overseas Edition) 8 63
[14] Emadzadeh A A, Speyer J 2011 Navigation in Space by X-ray Pulsars (London: Springer)
[15] Huang L W 2013 Ph. D. Dissertation (Beijing: Tsinghua University) (in Chinese) [黄良伟 2013 博士学位论文 (北京: 清华大学)]
[16] Taylor J H 1992 Phil. Trans. R. Soc. Lond. A 341 117
[17] Edwards R T, Hobbs G B, Manchester R N 2006 MNAS 372 1549
[18] Downs G S, Reichley P E 1983 Astrophys. J. (Supplement Series) 53 169
[19] Zhou Q Y, Ji J F, Ren H F 2014 Acta Phys. Sin. 62 139701 (in Chinese) [周庆勇, 姬剑锋, 任红飞 2013 62 139701]
[20] Scott D M, Finger H M, Wilson E A 2003 MNAS 344 412
[21] Dolch T, Lam M T, Cordes J, et al. 2014 Astrophys. J. 794 21
[22] Graven P, Collins J, Sheikh S I, et al. 2008 31st Annual AAS Guidance and Control Conference Breckenridge, Colorado, February 1-6, 2008 AAS 08-054
[23] Peng B, Jin C J, Du B, et al. 2012 Sci. China G 42 1292 (in Chinese) [彭勃, 金乘进, 杜彪, 等 2012 中国科学: 物理学 力学 天文学 42 1292]
[24] Nan R D 2005 Sci. China G 35 449 (in Chinese) [南仁东 2005 中国科学: 物理学 力学 天文学 35 449]
[25] Shen Z Q 2013 Science (KEXUE) 63 15 (in Chinese) [沈志强 2013 科学 63 15]
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