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Title:
A new technique for timing the double pulsar system
Authors:
Freire, P. C. C.; Wex, N.; Kramer, M.; Lorimer, D. R.; McLaughlin, M. A.; Stairs, I. H.; Rosen, R.; Lyne, A. G.
Affiliation:
AA(Arecibo Observatory, HC3 Box 53995, Arecibo, PR 00612, USA; Department of Physics, West Virginia University, PO Box 6315 Morgantown, WV 26506-6315, USA), AB(Max-Planck Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany), AC(Max-Planck Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany; University of Manchester, Jodrell Bank Centre for Astrophysics, Alan-Turing Building, Oxford Road, Manchester, M13 9PL), AD(Department of Physics, West Virginia University, PO Box 6315 Morgantown, WV 26506-6315, USA), AE(Department of Physics, West Virginia University, PO Box 6315 Morgantown, WV 26506-6315, USA), AF(University of British Columbia, 6224 Agricultural Road Vancouver, BC V6T 1Z1 Canada; ATNF, PO Box 76, Epping NSW 1710, Australia), AG(NRAO, Green Bank, WV 24944-0002, USA), AH(University of Manchester, Jodrell Bank Centre for Astrophysics, Alan-Turing Building, Oxford Road, Manchester, M13 9PL)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 396, Issue 7, pp. 1764-1770. (MNRAS Homepage)
Publication Date:
07/2009
Origin:
MNRAS
MNRAS Keywords:
binaries: general , pulsars: general , pulsars: individual: PSR J0737-3039A , pulsars: individual: PSR J0737-3039B
DOI:
10.1111/j.1365-2966.2009.14862.x
Bibliographic Code:
2009MNRAS.396.1764F

Abstract

In 2004, McLaughlin et al. discovered a phenomenon in the radio emission of PSR J0737-3039B (B) that resembles drifting subpulses. The repeat rate of the subpulses is equal to the spin frequency of PSR J0737-3039A (A); this led to the suggestion that they are caused by incidence upon B's magnetosphere of electromagnetic radiation from A. Here, we describe a geometrical model which predicts the delay of B's subpulses relative to A's radio pulses. We show that measuring these delays is equivalent to tracking A's rotation from the point of view of a hypothetical observer located near B. This has three main astrophysical applications: (i) to determine the sense of rotation of A relative to its orbital plane, (ii) to estimate where in B's magnetosphere the radio subpulses are modulated and (iii) to provide an independent estimate of the mass ratio of A and B. The latter might improve existing tests of gravitational theories using this system.
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