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Modelling X-ray Pulse Profiles of Millisecond Pulsars

Published online by Cambridge University Press:  20 March 2013

D. A. Leahy ,
S. Morsink  and
W. Tian
D. A. Leahy
Affiliation:
Dept. of Physics and Astronomy, University of Calgary, Calgary, CanadaT2N 1N4 email: [email protected]
S. Morsink
Affiliation:
Dept. of Physics, University of Alberta, Edmonton, Canada email: [email protected]
W. Tian
Affiliation:
National Astronomical Observatories, CAS, Beijing 100012, China email: [email protected]
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Abstract

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The modelling of X-ray pulse profiles from accreting millisecond pulsars is a way to infer masses and radii of neutron stars. We briefly describe how a pulse shape encodes information on the mass and radius, but also depends on other parameters such as hot spot location and observer viewing angle. A numerical model that we have developed is then described. The model includes light bending, time-delay effects, and Doppler effects for photons. The model accounts for oblateness of the neutron star, caused by the rapid rotation, and for scattered light from the surface of the accretion disk. The millisecond pulsar SAX J1808-3658 has multiple observations taken during different outbursts. The observed pulse shapes vary greatly, and it is a challenging test to fit the different observations. Some of the latest results are given.

Keywords

dense matterequation of stategravitational lensingstars: neutron
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. 441 - 443
Copyright
Copyright © International Astronomical Union 2013

References

Leahy, D. A. 2004, ApJ, 613, 517Google Scholar
Lattimer, J. M. & Prakash, M. 2007, Physics Reports, 442, 109Google Scholar
Cadeau, C., Leahy, D. A., & Morsink, S. M. 2005, ApJ, 618, 451CrossRefGoogle Scholar
Cadeau, C., Morsink, S. M., Leahy, D., & Campbell, S. S. 2007, ApJ, 654, 458Google Scholar
Morsink, S. M., Leahy, D. A., Cadeau, C., & Braga, J. 2007, ApJ, 663, 1244Google Scholar
Leahy, D. A., Morsink, S. M., & Cadeau, C. 2008, ApJ, 672, 1119CrossRefGoogle Scholar
Leahy, D. A., Morsink, S. M., Chung, Y.-Y., & Chou, Y. 2009, ApJ, 691, 1235Google Scholar
Morsink, S. M. & Leahy, D. A. 2011, ApJ, 726, 56Google Scholar
Leahy, D. A., Morsink, S. M., & Chou, Y. 2011, ApJ, 742, 17Google Scholar
Hartman, J. M., Patruno, A., Chakrabarty, D., et al. 2008, ApJ, 675, 1468CrossRefGoogle Scholar