Hostname: page-component-6bf8c574d5-h6jzd Total loading time: 0.001 Render date: 2025-02-22T05:54:39.275Z Has data issue: false hasContentIssue false
  • English
  • Français

PSR J1913+1102: a pulsar in a highly asymmetric and relativistic double neutron star system

Published online by Cambridge University Press:  04 June 2018

Robert D. Ferdman  and
the PALFA collaboration
Robert D. Ferdman
Affiliation:
Faculty of Science, University of East Anglia Norwich Research Park, Norwich NR4 7TJ, United Kingdom email: [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

PSR J1913+1102 is a double neutron star system (DNS) discovered in the Pulsar Arecibo L-band Feed Array survey. We have now very precisely measured the rate of advance of periastron for the system and the Einstein delay. From general relativity, this results in precise mass measurements: 1.65 ± 0.05 and 1.24 ± 0.05 M⊙ for the pulsar and neutron-star companion, respectively. This makes PSR J1913+1102 both the most massive double neutron star system known, and the most asymmetric in mass among compact DNS binaries. This asymmetry will allow for stringent limits on the effects of dipolar gravitational-wave radiation, predicted by alternative theories of gravity, as well as insight into heavy-element production from the eventual merger of this system and others like it. Further observations will also tighten constraints on formation and evolution models; this is crucial for understanding the DNS population, for which there are relatively few mass measurements.

Keywords

(stars:) pulsars: general (stars:) pulsars: individual (PSR J1913+1102)stars: neutron(stars:) binaries (including multiple): closerelativitygravitation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 13 , Symposium S337: Pulsar Astrophysics the Next Fifty Years , September 2017 , pp. 146 - 149
Copyright
Copyright © International Astronomical Union 2018 

References

Antoniadis, J., et al. 2013, Science, 340, 448Google Scholar
Bhat, R., Bailes, M., & Verbiest, J., 2008, Phys. Rev. D, 77, 124017CrossRefGoogle Scholar
Cordes, J. M. and Lazio, T. J. W. 2003, arXiv:astro-ph/0301598Google Scholar
Deller, A. T., Bailes, M., & Tingay, S. J., 2009, Science, 323, 1327Google Scholar
Esposito-Farese, G. 2005, in Novello, M., Bergliaffa, S. Perez, and Ruffini, R., editors, The Tenth Marcel Grossmann Meeting, page 647. World Scientific Publishing, 2005.Google Scholar
Ferdman, R. D., et al. 2013, ApJ, 767, 85CrossRefGoogle Scholar
Ferdman, R. D., et al. 2014, MNRAS, 443, 2183CrossRefGoogle Scholar
Freire, P. C. C., et al. 2012, MNRAS, 423, 3328Google Scholar
Just, O., et al. 2015, MNRAS, 448, 541Google Scholar
Kramer, M., et al. 2006, Science, 314, 97CrossRefGoogle Scholar
Lazarus, P., et al. 2016, ApJ, 831, 150Google Scholar
Lyne, A. G., et al. 2004, Science, 303, 1153CrossRefGoogle Scholar
Tanvir, N. R., et al. 2013, Nature, 500, 547Google Scholar
Tauris, T. M., et al. 2017, ApJ, 846, 170Google Scholar