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PSR J1906+0746: From relativistic spin-precession to beam modeling

Published online by Cambridge University Press:  20 March 2013

Gregory Desvignes ,
Michael Kramer ,
Ismaël Cognard ,
Laura Kasian ,
Joeri van Leeuwen ,
Ingrid Stairs  and
Gilles Theureau
Gregory Desvignes
Affiliation:
Max-Planck-Institut für Radioastronomie, Auf dem Hügel, 69 D-53121 Bonn, Germany email: [email protected]
Michael Kramer
Affiliation:
Max-Planck-Institut für Radioastronomie, Auf dem Hügel, 69 D-53121 Bonn, Germany email: [email protected]
Ismaël Cognard
Affiliation:
Laboratoire de Physique et Chimie de l'Environnement et de l'Espace, 3A Avenue de la Recherche Scientifique, 45071 Orléans cedex 2, France
Laura Kasian
Affiliation:
Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, BC V6T 1Z1, Canada
Joeri van Leeuwen
Affiliation:
ASTRON, the Netherlands Institute for Radio Astronomy, Postbus 2, 7990 AA Dwingeloo, The Netherlands
Ingrid Stairs
Affiliation:
Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, BC V6T 1Z1, Canada
Gilles Theureau
Affiliation:
Station de radioastronomie de Nançay, Observatoire de Paris, CNRS/INSU, 18330 Nançay, France
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Abstract

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Shortly after the discovery of PSR J1906+0746, some hints of profile variations were already interpreted as first signs of relativistic spin-precession occuring. Using observations from the Nançay, Arecibo and Green Bank Radio Observatories, we report here the measurement of pulse profile and polarimetric variations. Using the Rotating Vector Model, we show that PSR J1906+0746 is likely to be an orthogonal rotator (α ≃ 80°). Fitting our polarimetric data to a precession model, we determined the geometry of the pulsar and found a wide misalignment angle (δ = 89−44+85 deg, 95% C.L.), although the uncertainty is large. Assuming this geometry, we constructed the beam maps of both magnetic poles.

Keywords

pulsars: individual (J1906+0746)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S291: Neutron Stars and Pulsars: Challenges and Opportunities after 80 years , August 2012 , pp. 199 - 202
Copyright
Copyright © International Astronomical Union 2013

References

Barker, B. M. & O'Connell, R. F. 1975, ApJ, 199, L25Google Scholar
Damour, T. & Ruffini, R. 1974, Academie des Sciences Paris Comptes Rendus Serie Sciences Mathematiques 279 971–973Google Scholar
Desvignes, G. 2009, Thèse de doctorat, Université d'OrléansGoogle Scholar
Kasian, L. 2008, American Institute of Physics Conference Series, 983Google Scholar
Kasian, L. 2012, PhD thesis, University of British ColumbiaGoogle Scholar
Kramer, M. & Wex, N. 2009, Classical and Quantum Gravity, 26, 073001CrossRefGoogle Scholar
Lorimer, D. & Kramer, M. 2005, Handbook of Pulsar AstronomyGoogle Scholar
Lorimer, D. R. & Stairs, I. H. and Freire, P. C. C.et al. 2006, ApJ 640 428–434CrossRefGoogle Scholar
Lyne, A., Hobbs, G. & Kramer, et al. 2010, Science 329 408CrossRefGoogle Scholar
Manchester, R. N., Kramer, M., Stairs, I. H.et al. 2010, ApJ 710 1694–1709CrossRefGoogle Scholar
Radhakrishnan, V. & Cooke, D. J. 1969, ApL 3 225–229Google Scholar