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Recycling Pulsars: spins, masses and ages

Published online by Cambridge University Press:  20 March 2013

T. M. Tauris ,
M. Kramer  and
N. Langer
T. M. Tauris*
Affiliation:
Argelander-Institut für Astronomie, Universität Bonn, Germany Max-Planck Institut für Radioastronomie, Bonn, Germany
M. Kramer
Affiliation:
Max-Planck Institut für Radioastronomie, Bonn, Germany
N. Langer
Affiliation:
Argelander-Institut für Astronomie, Universität Bonn, Germany
*
*email: [email protected]
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Abstract

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Although the first millisecond pulsars (MSPs) were discovered 30 years ago we still do not understand all details of their formation process. Here, we present new results from Tauris, Langer & Kramer (2012) on the recycling scenario leading to radio MSPs with helium or carbon-oxygen white dwarf companions via evolution of low- and intermediate mass X-ray binaries (LMXBs, IMXBs). We discuss the location of the spin-up line in the PṖ–diagram and estimate the amount of accreted mass needed to obtain a given spin period and compare with observations. Finally, we constrain the true ages of observed recycled pulsars via calculated isochrones in the PṖ–diagram.

Keywords

stars: neutronpulsars: generalwhite dwarfsX-rays: binaries
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. 137 - 140
Copyright
Copyright © International Astronomical Union 2013

References

Alpar, M. A., Cheng, A. F., Ruderman, M. A., & Shaham, J. 1982, Nature, 300, 728Google Scholar
Bates, S. D., et al. 2011, MNRAS, 416, 2455Google Scholar
Bhattacharya, D. & van den Heuvel, E. P. J. 1991, Physics Reports, 203, 1CrossRefGoogle Scholar
Camilo, F., Thorsett, S. E., & Kulkarni, S. R. 1994, ApJ, 421, L15CrossRefGoogle Scholar
Freire, P. C. C., et al. 2011, Science, 334, 1107Google Scholar
Kiziltan, B. & Thorsett, S. E. 2010, ApJ, 715, 335Google Scholar
Spitkovsky, A. 2006, ApJ, 648, L51Google Scholar
Tauris, T. M., Langer, N., & Kramer, M. 2012, MNRAS, 425, 1601Google Scholar
Tauris, T. M. 2012, Science, 335, 561Google Scholar