Hostname: page-component-6bf8c574d5-956mj Total loading time: 0 Render date: 2025-02-20T12:31:41.844Z Has data issue: false hasContentIssue false
  • English
  • Français

Advances in our understanding of the free precession candidate PSR B1828-11

Published online by Cambridge University Press:  04 June 2018

G. Ashton ,
D. I. Jones  and
R. Prix
G. Ashton
Affiliation:
Max Planck Institut für Gravitationsphysik (Albert Einstein Institut) and Leibniz Universität Hannover, 30161 Hannover, DE email: [email protected]
D. I. Jones
Affiliation:
Mathematical Sciences, University of Southampton, Southampton SO17 1BJ, UK
R. Prix
Affiliation:
Max Planck Institut für Gravitationsphysik (Albert Einstein Institut) and Leibniz Universität Hannover, 30161 Hannover, DE email: [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We highlight the advances and difficulties in understanding PSR B1828-11, which undergoes long-term periodic modulations in its timing and pulse shape over several years. A model comparison of precession and magnetospheric switching models based on the long-term modulation data favours the former; we discuss the implications of this in the context of short timescale switching observed in this pulsar. Furthermore, we highlight the difficulties this pulsar poses for our understanding of pulsars due to the increasing rate of the modulation period and its behaviour during a recent glitch.

Keywords

pulsars: individual (PSR B1828-11)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 13 , Symposium S337: Pulsar Astrophysics the Next Fifty Years , September 2017 , pp. 307 - 308
Copyright
Copyright © International Astronomical Union 2018 

References

Akgün, T., Link, B., & Wasserman, I. (2006). MNRAS, 365:653–672.Google Scholar
Ashton, G., Jones, D. I., & Prix, R. (2016). MNRAS, 458:881–899.Google Scholar
Ashton, G., Jones, D. I., & Prix, R. (2017). MNRAS, 467:164–178.Google Scholar
Bailes, M., Lyne, A. G., & Shemar, S. L. (1993). In Phillips, J. A., Thorsett, S. E., and Kulkarni, S. R., editors, Planets Around Pulsars, volume 36 of Astronomical Society of the Pacific Conference Series, page 19.Google Scholar
Cordes, J. M. (2013). ApJ, 775:47.Google Scholar
Espinoza, C. M., Lyne, A. G., Stappers, B. W., & Kramer, M. (2011). MNRAS, 414:1679.Google Scholar
Hobbs, G., Lyne, a. G., & Kramer, M. (2010). MNRAS, 402 (2):1027–1048.Google Scholar
Jones, D. I. (2012). MNRAS, 420:2325–2338.Google Scholar
Jones, D. I., Ashton, G., & Prix, R. (2017). Phys. Rev. Lett., 118 (26):261101.Google Scholar
Kerr, M., Hobbs, G., Johnston, S., & Shannon, R. M. (2016). MNRAS, 455:1845–1854.CrossRefGoogle Scholar
Lyne, A., Hobbs, G., Kramer, M., Stairs, I., & Stappers, B. (2010). Science, 329:408.Google Scholar
Perera, B. B. P., Stappers, B. W., Weltevrede, P., Lyne, A. G., & Bassa, C. G. (2015). MNRAS, 446:1380–1388.Google Scholar
Stairs, I. H., Athanasiadis, D., Kramer, M., & Lyne, A. G. (2003). In Bailes, M., Nice, D. J., and Thorsett, S. E., editors, Radio Pulsars, volume 302 of Astronomical Society of the Pacific Conference Series, page 249.Google Scholar
Stairs, I. H., Lyne, A. G., & Shemar, S. L. (2000). Nature, 406:484.Google Scholar
Weisberg, J. M., Everett, J. E., Cordes, J. M., Morgan, J. J., & Brisbin, D. G. (2010). ApJ, 721 (2):1044.Google Scholar