Study on autonomous navigation based on pulsar timing model

Article

Abstract

The basic principle of pulsar timing model was introduced, and the general relativistic corrections were analyzed when pulse time of arrival (TOA) was transferred to coordinate TOA at the Solar System Barycentre. Based on the shifting, an iterative method of autonomous position determination for spacecraft was developed. Accordingly, the linear form of the position offset equation was evolved. Using the initial estimated value of spacecraft’s position as the input of pulsar timing equation, through calculation of the offset between measured or transferred and predicted TOA, the position offset can be solved by Least Squares. At last, the main error sources including modeling error and parameters error were discussed.

Keywords

X-ray pulsar pulsar timing model autonomous navigation TOA measurement 

Preview

Unable to display preview. Download preview PDF.

Unable to display preview. Download preview PDF.

References

  1. 1.
    Joseph H, Taylor J R. Millisecond pulsars: Nature’s most stable clocks. Proc IEEE, 1991, 79(7): 1054–1062[DOI]CrossRefADSGoogle Scholar
  2. 2.
    Moyer T D. Formulation for Observed and Computed Values of Deep Space Network Data Types. California: JPL Publication, 2000. 8–9Google Scholar
  3. 3.
    Backer D C, Hellings R W. Pulsar timing and general relativity. Annu Rev Astron Astrophy, 1986, 24: 537–575[DOI]CrossRefADSGoogle Scholar
  4. 4.
    Martin C F, Torrence M H, Misner C W. Relativistic effects on an earth-orbiting satellite in the barycenter coordinate system. J Geophy Res, 1985, 90(B1): 9403–9410[DOI]CrossRefADSGoogle Scholar
  5. 5.
    Lorimer D R, Kramer M. Handbook of Pulsar Astronomy. Cambridge: Cambridge University Press, 2005. 205Google Scholar
  6. 6.
    Hotan A W. High-Precision Observations of Relativistic Binary and Millisecond Pulsars. Doctoral Dissertation. Melbourne: Swinburne University of Technology, 2006. 27–29Google Scholar
  7. 7.
    Sheikh S I, Pines D J. Spacecraft navigation using x-ray pulsars. J Guid Contr Dyn, 2006, 29(1): 49–61[DOI]CrossRefGoogle Scholar
  8. 8.
    Hellings R W. Relativistic effects in astronomical timing measurements. Astron J, 1986, 91(3): 650–659[DOI]CrossRefADSGoogle Scholar
  9. 9.
    Thomas J B. Reformation of the relativistic conversion between coordinate time and atomic time. Astron J, 1975, 80(5): 405–411 [DOI]CrossRefGoogle Scholar
  10. 10.
    Moyer T D. Transmation from proper time on earth to coordinate time in solar system barycentric space-time frame of reference, Part I. Celestl Mech, 1981, 23: 33–56[DOI]MATHCrossRefADSMathSciNetGoogle Scholar
  11. 11.
    Moyer T D. Transmation from proper time on earth to coordinate time in solar system barycentric space-time frame of reference, Part II. Celest Mech, 1981, 23: 57–68[DOI]MATHCrossRefADSMathSciNetGoogle Scholar
  12. 12.
    Taylor J H, Weisberg J M. Further experimental tests of relativistic gravity using the binary pulsar PSR, 1913+16. Astrophys J, 1989, 345: 434–450[DOI]CrossRefADSGoogle Scholar
  13. 13.
    Shapiro I I. Fourth test of general relativity. Phys Rev Lett, 1964, 13(26): 163–174CrossRefADSGoogle Scholar
  14. 14.
    Edwards R T, Hobbs G B, Manchaester R N. Tempo2, a new pulsar timing package: II. The timing model and precision estimates. Mon Not Roy Astron Soc, 2006, 372: 1549–1574[DOI]CrossRefADSGoogle Scholar
  15. 15.
    Nan R D. Five hundred meter aperture spherical radio telescope (FAST). Sci China Ser G-Phys Mech Astron, 2006, 49: 129–148 [DOI]CrossRefADSGoogle Scholar

Copyright information

© Science in China Press and Springer-Verlag GmbH 2009

Authors and Affiliations

  1. 1.School of Automation and Information EngineeringXi’an University of TechnologyXi’anChina

Personalised recommendations