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Changes in Polarization Position Angle across the Eclipse in the Double Pulsar System

Published online by Cambridge University Press:  20 March 2013

R. Yuen ,
R. N. Manchester ,
M. Burgay ,
F. Camilo ,
M. Kramer ,
D. B. Melrose  and
I. H. Stairs
R. Yuen
Affiliation:
CSIRO Astronomy and Space Science, Australia Telescope National Facility, P.O. Box 76, Epping, NSW 1710, Australia SIfA, School of Physics, the University of Sydney, NSW 2006, Australia
R. N. Manchester
Affiliation:
CSIRO Astronomy and Space Science, Australia Telescope National Facility, P.O. Box 76, Epping, NSW 1710, Australia
M. Burgay
Affiliation:
INAF-Osservatorio Astronomica di Cagliari, Loc. Poggio dei Pini, Strada 54, 09012 Capoterra, Italy
F. Camilo
Affiliation:
Columbia Astrophysics Laboratory, Columbia University, New York, NY 10027, USA
M. Kramer
Affiliation:
Max Planck Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
D. B. Melrose
Affiliation:
SIfA, School of Physics, the University of Sydney, NSW 2006, Australia
I. H. Stairs
Affiliation:
Department of Physics and Astronomy, University of British Columbia, Vancouver, BC V6T 1Z1, Canada
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Abstract

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We investigate the changes in polarization position angle in radiation from pulsar A around the eclipse in the Double Pulsar system PSR J0737-3039A/B at the 20 cm and 50 cm wavelengths using the Parkes 64-m radio telescope. The changes are ~ 2σ during and shortly after the eclipse at 20 cm but less significant at 50 cm. We show that the changes in position angle during the eclipse can be modelled by differential synchrotron absorption in the eclipse regions. Position angle changes after the eclipse are interpreted as Faraday rotation in the magnetotail of pulsar B. Implied charge densities are consistent with the Goldreich-Julian density, suggesting that the particle energies in the magnetotail are mildly relativistic.

Keywords

binaries: eclipsing — polarization — pulsars: individual (PSR J0737-3039A, PSR J0737-3039B)
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. 580 - 582
Copyright
Copyright © International Astronomical Union 2013

References

Arons, J., Backer, D. C., Spitkovsky, A., & Kaspi, V. M. 2004, Proc. 2004 Apsen Winter Conf. on Astrophysics, Binary Radio Pulsars, San Francisco: ASPGoogle Scholar
Goldreich, P. & Julian, W. H. 1969, ApJ, 157, 869CrossRefGoogle Scholar
Hotan, A. W., van Straten, W., & Manchester, R. N. 2004, Publications of the Astronomcial Society of Australia, 21, 302CrossRefGoogle Scholar
Lyne, A. G., Burgay, M., Kramer, M., Possenti, A., Manchester, R. N.et al. 2004, Science, 303, 1153CrossRefGoogle Scholar
Lyutikov, M. & Thompson, C. 2005, ApJ, 634, 1223CrossRefGoogle Scholar
Manchester, R. N., Kramer, M., Stairs, I. H., Burgay, M., Camilo, F., Hobbs, G. B., Lorimer, D. R., Lyne, A. G., McLaughlin, M. A. McPhee. A., Possenti, A., Reynolds, J. E., & van Straten, W. 2010, ApJ, 710, 1694CrossRefGoogle Scholar
Spitkovsky, A. & Arons, J. 2004, Bulletin of the American Astronomical Society, HEAD meeting, 36 (8, 08.02), 917Google Scholar
Weise, J. I. & Melrose, D. B. 2002, MNRAS, 329, 115Google Scholar