Astrophysics and Space Science

, Volume 213, Issue 1, pp 135–138 | Cite as

Evidence of pulsed X-ray emission from radio pulsar PSR1951+32

(Letter to the Editor)
  • Lingxiang Cheng
  • Tipei Li
  • Xuejun Sun
  • Yuqian Ma
  • Mei Wu
Article
Received:
  • 33 Downloads

Abstract

Evidence of X-ray pulsations from PSR 1951+32 have been obtained in bothEinstein IPC (Image Proportional Counter) and HRI(High Resolution Imager) data in our analysis of Einstein Observatory data on CTB 80 area. The phase light curves of these two datasets show similar single peak structure. The period values are significantly different from those predicted by radio observations processed about 7 years later, and shows the spin rate of the pulsar in April 1980 is higher than that in October 1979. Possible explanations for this phenomenon are discussed.

Keywords

Observatory Data Resolution Imager Single Peak Light Curf High Resolution Imager 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.
This is a preview of subscription content, log in to check access.

Preview

Unable to display preview. Download preview PDF.

Unable to display preview. Download preview PDF.

References

  1. Angellini, L.et al.: 1988,Astrophys. J. 330, L43.Google Scholar
  2. Angerhofer, P.E.et al.: 1981,Astron. Astrophys. 94, 313.Google Scholar
  3. Angerhofer, P.E., Wilson, A.S. and Mould, J.R.: 1980,Astrophys. J. 236, 143.Google Scholar
  4. Becker, R.H., Helfand, D.J. and Szymkowiak, A.E.: 1982,Astrophys. J. 255, 557.Google Scholar
  5. Blair, W.P.et al.: 1984,Astrophys. J. 282, 161.Google Scholar
  6. Blair, W.P. and Schild, R.E.: 1985,Astrophys. Lett. 24, 189.Google Scholar
  7. Buccheri, R.et al.: 1983,Astron. Astrophys. 128, 245.Google Scholar
  8. Clifton, T.R.et al.: 1987,IAU Circ. No.4422.Google Scholar
  9. Davelaar, J., Smith, A., and Becker, R.H.: 1986,Astrophys. J. 300, L59.Google Scholar
  10. Dickle, J.R.et al.: 1981,Vistas Astron. 25, 127.Google Scholar
  11. Fesen, R.A. and Gull, T.R.: 1985,Astrophys. Lett. 24, 197.Google Scholar
  12. Foster, R.S., Backer, D.C. and Wolszczan A.: 1990,Astrophys. J. 356, 243.Google Scholar
  13. Fruchter, A.S.et al.: 1988,Nature 331, 53.Google Scholar
  14. Li, J.D.et al.: 1987,IAU Circ. No.4492.Google Scholar
  15. Li, T.P.et al.: 1990,Acta Astrophys. Sinica 10, 298.Google Scholar
  16. Lu, T. and Shi, T.Y.: 1990,Astron. Astrophys. 231, L7.Google Scholar
  17. Mantovani, F.et al.: 1985,Astron. Astrophys. 145, 50.Google Scholar
  18. Ögelman, H. and Buccheri, R.: 1987,Astron. Astrophys. 186, L17.Google Scholar
  19. Storm, R.G., Angerhofer, P.E. and Velusarny, T.: 1980,Nature 284, 38.Google Scholar
  20. Storm, R.G. and Blair, W.P.: 1985,Astron. Astrophys. 149, 259.Google Scholar
  21. van den Bergh, S.: 1980,Publ. Astron. Soc. Pacific 92, 768.Google Scholar
  22. Velusalry, T. and Kundu, M.R.: 1974,Astron. Astrophys. 32, 375.Google Scholar
  23. Velusamy, T., Kundu, M.R. and Becker, R.H.: 1976,Astron. Astrophys. 51, 21.Google Scholar
  24. Wang, Z.R. and Seward, F.D.: 1984,Astrophys. J. 285, 607.Google Scholar
  25. White, N.E. and Stella, L.: 1988,Nature 332, 416.Google Scholar

Copyright information

© Kluwer Academic Publishers 1994

Authors and Affiliations

  • Lingxiang Cheng
    • 1
  • Tipei Li
    • 1
  • Xuejun Sun
    • 1
  • Yuqian Ma
    • 1
  • Mei Wu
    • 1
  1. 1.High Energy Astrophysics LabInstitute of High Energy PhysicsBeijingChina

Personalised recommendations