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Population synthesis of young neutron stars

Published online by Cambridge University Press:  20 March 2013

Andrei P. Igoshev  and
Alexander F. Kholtygin
Andrei P. Igoshev
Affiliation:
Institute of Astronomy, Saint Petersburg State University email: ignotur@gmail.com
Alexander F. Kholtygin
Affiliation:
Institute of Astronomy, Saint Petersburg State University email: ignotur@gmail.com
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Abstract

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We investigate the fortune of young neutron stars (NS) in the whole volume of the Milky Way with new code for population synthesis. We start our modeling from the birth of massive OB stars and follow their motion in the Galaxy up to the Supernova explosion. Next we integrate the equations of motion of NS in the averaged gravitational potential of the Galaxy. We estimate the mean kick velocities from a comparison the model Z and R-distributions of radio emitting NS with that for galactic NS accordingly ATNF pulsar catalog. We follow the history of the rotational velocity and the surface magnetic field of NS taking into account the significant magnetic field decay during the first million year of a neutron star's life. The derived value for the mean time of ohmic decay is 2.3ċ105 years. We model the subsample of galactic radio pulsars which can be detected with available radio telescopes, using a radio beaming model with inhomogeneous distribution of the radio emission in the cone. The distributions functions of the pulsar periods P, period derivatives Ṗ and surface magnetic fields B appear to be in a close agreement with those obtained from an ensemble of neutron stars in the ATNF catalogue.

Keywords

methods: data analysismethods: statisticalstars: neutronmagnetic fieldspulsars: general
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. 411 - 413
Copyright
Copyright © International Astronomical Union 2013

References

Manchester, R. N., Hobbs, G. B., Teoh, A., & Hobbs, M. 2005, AJ, 129, 1993Google Scholar
Cordes, J. M. & Lazio, T. J. W. 2002, ArXiv:0207156Google Scholar
Lorimer, D. R., Faulkner, A. J., Lyne, A. G., Manchester, R. N., Kramer, M., McLaughlin, M. A., Hobbs, G., Possenti, A., Stairs, I. H., Camilo, F., Burgay, M., D'Amico, N., Corongiu, A., & Crawford, F., 2002, MNRAS 372, 777–800CrossRefGoogle Scholar
Faucher-Giguere, C. A. & Kaspi, V. M. 2006, ApJ 643, 1, 332–355CrossRefGoogle Scholar
Popov, S. B., Pons, J. A., Miralles, J. A., Boldin, P. A., & Posselt, B. 2010, MNRAS 401, 4, 2675–2686Google Scholar
Igoshev, A. P. & Kholtygin, A. F. 2011, AN 332, 9/10, 1012Google Scholar
Maciesiak, K. & Gil, J. 2011, MNRAS 417, 2, 1444–1453Google Scholar
Rankin, J. M. 1990, ApJ 352, 247–257Google Scholar