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Heavy Neutron Stars? A Status Report on Arecibo Timing of Four Pulsar – White Dwarf Systems

Published online by Cambridge University Press:  19 July 2016

David J. Nice ,
Eric M. Splaver  and
Ingrid H. Stairs
David J. Nice
Affiliation:
Physics Department, Princeton University Box 708, Princeton, NJ 08544 USA
Eric M. Splaver
Affiliation:
Physics Department, Princeton University Box 708, Princeton, NJ 08544 USA
Ingrid H. Stairs
Affiliation:
Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, BC V6T 1Z1, Canada

Abstract

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Relativistic phenomena (orbital precession, Shapiro delay, and/or orbital decay) have been measured in Arecibo timing observations of four pulsar-white dwarf binaries, leading to constraints on the neutron star masses. We have detected the decay of the PSR J0751+1807 orbit due to gravitational radiation emission, the first such measurement in a binary with a low mass ratio (m2/m1 ≪ 1). Timing data constrains the mass of this pulsar to bet between 1.6 and 2.8 M⊙. Masses of the other pulsars are in marginal agreement with the canonical pulsar mass of 1.35 M⊙, but higher values are preferred.

Type
Part 1: Neutron Star Formation and Evolution
Information
Symposium - International Astronomical Union , Volume 218: Young Neutrons Stars and their Environments , 2004 , pp. 49 - 52
Copyright
Copyright © Astronomical Society of the Pacific 2004 

References

Arzoumanian, Z. 2003, in ASP Conf. Series, Vol. 302, Radio Pulsars, eds. Bailes, M. et al., (San Francisco: ASP), p. 69.Google Scholar
Bailes, M, Ord, S. M., Knight, H. S., & Hotan, A W. 2003, ApJ, 595, 49.CrossRefGoogle Scholar
Brown, G. E. 1995, ApJ, 440, 270.CrossRefGoogle Scholar
Deich, W. T. S., & Kulkarni, S. R. 1996, in IAU Symp. 165, Compact Stars in Binaries, eds. van Paradijs, J. et al., (Dordrecht: Kluwer), p. 279.CrossRefGoogle Scholar
Kaspi, V. M., Taylor, J. H., & Ryba, M. F. 1994, ApJ, 428, 713.CrossRefGoogle Scholar
Nice, D. J., Splaver, E. M., & Stairs, I. H. 2003, in ASP Conf. Series, Vol. 302, Radio Pulsars, eds. Bailes, M. et al., (San Francisco: ASP), p. 75.Google Scholar
Podsiadlowski, P., Rappaport, S., & Pfahl, E. D. 2002, ApJ, 565, 1107.CrossRefGoogle Scholar
Rappaport, S., et al. 1995, MNRAS, 273, 731.CrossRefGoogle Scholar
Splaver, E. M., et al. 2002, ApJ, 581, 509.CrossRefGoogle Scholar
Stairs, I. H., Thorsett, S. E., Taylor, J. H., & Wolszczan, A. 2002, ApJ, 581, 501.CrossRefGoogle Scholar
Tauris, T. M., & Savonije, G. J. 1999, A&A, 350, 928.Google Scholar
Taylor, J. H. 1992, Phil. Trans. R. Soc. Lond. A, 341, 117.CrossRefGoogle Scholar
Thorsett, S. E., & Chakrabarty, D. 1999, ApJ, 512, 288.CrossRefGoogle Scholar
Weisberg, J. M., & Taylor, J. H. 2003, in ASP Conf. Series, Vol. 302, Radio Pulsars, eds. Bailes, M. et al., (San Francisco: ASP), p. 93.Google Scholar
van Straten, W. et al. 2001, Nature, 412, 158.CrossRefGoogle Scholar