Hostname: page-component-586b7cd67f-l7hp2 Total loading time: 0 Render date: 2024-11-26T09:09:35.472Z Has data issue: false hasContentIssue false
  • English
  • Français

Correlated emission and spin-down variability in radio pulsars

Published online by Cambridge University Press:  04 June 2018

Benjamin Shaw ,
Benjamin W. Stappers ,
Paul R. Brook ,
Aris Karastergiou ,
Andrew G. Lyne  and
P. Weltevrede
Benjamin Shaw
Affiliation:
Jodrell Bank Centre for Astrophysics, The University of Manchester, Manchester, M13 9PL, UK email: [email protected]
Benjamin W. Stappers
Affiliation:
Jodrell Bank Centre for Astrophysics, The University of Manchester, Manchester, M13 9PL, UK email: [email protected]
Paul R. Brook
Affiliation:
Dept. of Physics and Astronomy, West Virginia University, P.O. Box 6315, Morgantown, WV 26505, USA
Aris Karastergiou
Affiliation:
Astrophysics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford, OX1 3RH, UK
Andrew G. Lyne
Affiliation:
Jodrell Bank Centre for Astrophysics, The University of Manchester, Manchester, M13 9PL, UK email: [email protected]
P. Weltevrede
Affiliation:
Jodrell Bank Centre for Astrophysics, The University of Manchester, Manchester, M13 9PL, UK 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.

The recent revelation that there are correlated period derivative and pulse shape changes in pulsars has dramatically changed our understanding of timing noise as well as the relationship between the radio emission and the properties of the magnetosphere as a whole. Using Gaussian processes we are able to model timing and emission variability using a regression technique that imposes no functional form on the data. We revisit the pulsars first studied by Lyne et al. (2010). We not only confirm the emission and rotational transitions revealed therein, but reveal further transitions and periodicities in 8 years of extended monitoring. We also show that in many of these objects the pulse profile transitions between two well-defined shapes, coincident with changes to the period derivative. With a view to the SKA and other telescopes capable of higher cadence we also study the detection limitations of period derivative changes.

Keywords

pulsars: generalstars: neutronmethods: data analysismethods: statistial
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 13 , Symposium S337: Pulsar Astrophysics the Next Fifty Years , September 2017 , pp. 58 - 61
Copyright
Copyright © International Astronomical Union 2018 

References

Brook, P. R., Karastergiou, A., Johnston, S., Kerr, M., Shannon, R. M. & Roberts, S. J., 2015, MNRAS, 456, 1374Google Scholar
Kramer, M., Lyne, A. G., O’Brien, J. T., Jordan, C. A., & Lorimer, D. R., 2006, Science, 312, 549Google Scholar
Hobbs, G., Lyne, A. G., & Kramer, M., 2010, MNRAS, 402, 1027Google Scholar
Lyne, A. G., Hobbs, G., Kramer, M., Stairs, I., & Stappers, B. W., 2010, Science, 329, 408CrossRefGoogle Scholar
Perera, B. B. P., Stappers, B. W., Weltevrede, P., Lyne, A. G., & Bassa, C. G., 2015, MNRAS, 446, 1380Google Scholar
Shaw, B., Stappers, B. W., Brook, P. R., Karastergiou, A., Lyne, A. G., & Weltevrede, P. 2018a, (in prep)Google Scholar
Shaw, B., Stappers, B. W., & Weltevrede, P. 2018b, (in prep)Google Scholar