Peculiarities of radio pulsars with long periods

Cover Page

Cite item

Full Text

Open Access Open Access
Restricted Access Access granted
Restricted Access Subscription Access

Abstract

The analysis of parameters of radio pulsars with periods P > 5 sec has been carried out. It was found that there is not a clear dependence dP / dt on P on the diagram {dP / dt, P}. Such lack of any dependence can be explained in the frame of the disk model. It is shown that the pulse width decreases with increasing period for the sample considered. It is the opposite of the dependence in the generally accepted pulsar model. Such a behavior can be explained by the dependence of the level of radiation on the period, The alternative explanation is a non-dipole structure of magnetic field in the region of the generation of observed radiation. We consider the possibility of the description of extremely long intervals between successive pulses in pulsars J0901–4046 and J0250+5854 using the model of drift waves at the periphery of the magnetosphere. In the drift model rotation periods of these pulsars are several times shorter than the intervals between observed pulses.

Full Text

Restricted Access

About the authors

I. F. Malov

P. N. Lebedev Physical Institute of Russian Academy of Sciences

Author for correspondence.
Email: malov@prao.ru

Astrospace Center, Pushchino Radio Astronomy Observatory

Russian Federation, Pushchino, Moscow region

References

  1. C. M. Tan, C. G. Bassa, S. Cooper, T. J. Dijkema, et al., 866(1), Astrophys. J. 54 (2018).
  2. M. Caleb, I. Heywood, K. Rajwade, M. Malenta, et al., Nature Astron. 6, 828 (2022), arXiv:2206.01346 [astro-ph.HE].
  3. K. Chen and M. Ruderman, Astrophys. J., 402, 264 (1993).
  4. И. Ф. Малов, Радиопульсары (М.: Наука, 2004).
  5. А. А. Логинов, И. Ф. Малов, Астрон. журн. 91(1), 57 (2014).
  6. А. А. Логинов, И. Ф. Малов, Астрон. журн. 91(10), 833 (2014).
  7. R. N. Manchester, G. B. Hobbs, A. Teoh, and M. Hobbs, Astron. J. 129(4), 1993 (2005).
  8. F. C. Michel and A. J. Dessler, Astrophys. J. 251, 654 (1981).
  9. В. Ф. Шварцман, Изв. ВУЗов. Радиофизика 13, 1852 (1970).
  10. A. Z. Kazbegi, G. Z. Machabeli, and G. I. Melikidze, Australian J. Physics 44, 573 (1991).
  11. A. Z. Kazbegi, G. Z. Machabeli, G. I. Melikidze, and C. Shukre, Astron. and Astrophys. 309, 515 (1996).
  12. D. Lomiashvili, G. Machabeli, and I. Malov, Astrophys. J. 637, 1010 (2002).
  13. Z. Wang, D. Chakrabarty, and D. L. Kaplan, Nature 440(7085), 772 (2006), arXiv:astro-ph/0604076.

Supplementary files

Supplementary Files
Action
1. JATS XML
Download
2. Fig. 1. Diagram of {dP/dt, P} in logarithmic scale for pulsars with P > 5 s.

Download (65KB)
Indexing metadata
3. Fig. 2. Dependence of the pulse width W10 on the period P for pulsars with P > 5 s.

Download (67KB)
Indexing metadata
4. Fig. 3. Dependence between the pulse widths at the 10% level (W10) and at half the intensity (W50) for pulsars with P > 5 s.

Download (64KB)
Indexing metadata
5. Fig. 4. Lines of force of the quadrupole magnetic field touching the light cylinder. The values ​​of r/rl c and angle θ are indicated.

Download (215KB)
Indexing metadata
6. Fig. 5. Oscillating radiation pattern [12] at ωdr = 2π /17 s–1, Ω = 2π / 0.85 s–1; t1 and t2 correspond to two consecutive periods of rotation P = 2π / Ω.

Download (125KB)
Indexing metadata

Copyright (c) 2024 The Russian Academy of Sciences