Search for interpulses in a complete sample of pulsars at a frequency of 111 MHz

Cover Page

Cite item

Full Text

Open Access Open Access
Restricted Access Access granted
Restricted Access Subscription or Fee Access

Abstract

An interpulse search was carried out in a sample of 96 pulsars observed on the Large Phased Array (LPA) radio telescope in the Pushchino Multibeams Pulsar Search (PUMPS). The pulsar sample is complete for pulsars having a signal-to-noise ratio (S/N) in the main pulse (MP) greater than 40. To search for weak interpulses (IP), the addition of average profiles over an interval of up to 10 years was used. Interpulses were detected in 12 pulsars (12.5% of the sample), of which 7 pulsars have an interpulse located near the 180◦ phase relative to the main pulse (probable orthogonal rotators), and 5 have phases far from 180◦ (probable coaxial rotators). The amplitude ratios of IP/MP are in the range of 0.004−0.023, the median value is 0.01. Estimates of the observed number of coaxial and orthogonal rotators with IP/MP ≥0.01 do not contradict the model according to which, during evolution, the magnetic axis and the axis of rotation become orthogonal.

Full Text

Restricted Access

About the authors

M. O. Toropov

LLC TEK Inform

Email: serg@prao.ru
Russian Federation, Moscow

S. A. Tyul’bashev

Lebedev Physical Institute

Author for correspondence.
Email: serg@prao.ru

Astro-Space Center, Pushchino radio astronomy observatory

Russian Federation, Pushchino

V. S. Beskin

Lebedev Physical Institute; Moscow Institute of Physics and Technology (MIPT)

Email: serg@prao.ru
Russian Federation, Moscow; Dolgoprudnyi

References

  1. R.N. Manchester, G.B. Hobbs, A. Teoh, and M. Hobbs, Astron. J. 129(4), 1993 (2005).
  2. J. Gil, Astron. and Astrophys. 127, 267 (1983).
  3. K. Maciesiak, J. Gil, and V.A.R.M. Ribeiro, Monthly Not. Roy. Astron. Soc. 414(2), 1314 (2011).
  4. D.R. Lorimer and M. Kramer, Handbook of Pulsar Astronomy (Cambridge, UK: Cambridge University Press, 2012).
  5. L. Davis and M. Goldstein, Astrophys. J. Letters 159, L81 (1970).
  6. R.N. Manchester and A.G. Lyne, Monthly Not. Roy. Astron. Soc. 181, 761 (1977).
  7. P. Goldreich, Astrophys. J. Letters 160, L11 (1970).
  8. A. Philippov, A. Tchekhovskoy, and J.G. Li, Monthly Not. Roy. Astron. Soc. 441(3), 1879 (2014).
  9. V.S. Beskin, A.V. Gurevich, and Y.N. Istomin, Physics of the Pulsar Magnetosphere (Cambridge, New York: Cambridge University Press, 1993).
  10. A.G. Lyne, C.A. Jordan, F. Graham-Smith, C.M. Espinoza, B.W. Stappers, and P. Weltevrede, Monthly Not. Roy. Astron. Soc. 446(1), 857 (2015).
  11. V.I. Shishov, I.V. Chashei, V.V. Oreshko, S.V. Logvinenko, et al., Astron. Rep. 60(12), 1067 (2016).
  12. S.A. Tyul’bashev, V.S. Tyul’bashev, V.V. Oreshko, and S.V. Logvinenko, Astron. Rep. 60(2), 220 (2016).
  13. S.A. Tyul’bashev, P.Y. Golysheva, V.S. Tyul’bashev, and I.A. Subaev, Astron. Rep. 63(11), 920 (2019).
  14. S.A. Tyul’bashev, M.A. Kitaeva, and G.E. Tyul’basheva, Monthly Not. Roy. Astron. Soc. 517(1), 1112 (2022).
  15. S.A. Tyul’bashev, G.E. Tyul’basheva, M.A. Kitaeva, I.L. Ovchinnikov, V.V. Oreshko, and S.V. Logvinenko, Monthly Not. Roy. Astron. Soc. 528(2), 2220 (2024).
  16. I.F. Malov and E.B. Nikitina, Astron. Rep. 57(11), 833 (2013).
  17. A.D. Kuz’min, B.Ya. Losovskii, and K.A. Lapaev, Astron. Rep. 51(8), 615 (2007).
  18. A.V. Pynzar’ and V.I. Shishov, Astron. Rep. 52(8), 623 (2008).
  19. P. Weltevrede and S. Johnston, Monthly Not. Roy. Astron. Soc. 387(4), 1755 (2008).
  20. P.F. Wang, J.L. Han, J. Xu, C. Wang, et al., Res. Astron. and Astrophys. 3(10), id. 104002 (2023).
  21. B. Posselt, A. Karastergiou, S. Johnston, A. Parthasarathy, et al., Monthly Not. Roy. Astron. Soc. 520(3), 4582 (2023).
  22. E.M. Novoselov, V.S. Beskin, A.K. Galishnikova, M.M. Rashkovetskyi, and A.V. Biryukov, Monthly Not. Roy. Astron. Soc. 494(3), 3899 (2020).
  23. L.I. Arzamasskiy, V.S. Beskin, and K.K. Pirov, Monthly Not. Roy. Astron. Soc. 466(2), 2325 (2017).
  24. A. Spitkovsky, Astrophys. J. Letters 648(1), L51 (2006).

Supplementary files

Supplementary Files
Action
1. JATS XML
Download
2. Fig. 1. There are 12 paired images, each of which shows the summed average profile of the pulsar in the upper part (the name of the pulsar is indicated in the upper right corner), and in the lower part the MP peak in the profile is removed so that the IP is visible. The arrows in the images indicate the positions of the MP and IP.

Download (498KB)
Indexing metadata

Copyright (c) 2024 The Russian Academy of Sciences