The evolution of PSR J0737-3039B and a model for relativistic spin precession

Perera, B. B. P., McLaughlin, M. A., Kramer, M., Stairs, I. H., Ferdman, R. D. ORCID: https://orcid.org/0000-0002-2223-1235, Freire, P. C. C., Possenti, A., Breton, R. P., Manchester, R. N., Burgay, M., Lyne, A. G. and Camilo, F. (2011) The evolution of PSR J0737-3039B and a model for relativistic spin precession. In: AIP Conference Proceedings. AIP Conference Proceedings, 1357 . American Institute of Physics, ITA. ISBN 978-0-7354-0915-6

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Abstract

We present the evolution of the radio emission from the 2.8-s pulsar of the double pulsar system PSR J0737-3039A/B. We describe the changes in the pulse profile and flux density over five years of observations, culminating in the B pulsar's radio disappearance in 2008 March. Over this time, the flux density decreased by 0.177 mJy yr(-1) at the brightest orbital phases and the pulse profile evolved from a single to a double peak. Relativistic spin precession, coupled with an elliptical beam, can model the pulse profile evolution well and the reappearance is expected to happen in similar to 2035 with the same part of the beam or in similar to 2014 if we assume a symmetric beam shape.

Item Type:	Book Section
Uncontrolled Keywords:	stars:neutron,pulsars,double-pulsar
Depositing User:	LivePure Connector
Date Deposited:	11 Jul 2018 09:30
Last Modified:	24 Sep 2024 08:10
URI:	https://ueaeprints.uea.ac.uk/id/eprint/67580
DOI:	10.1063/1.3615090

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