A Massive Pulsar in a Compact Relativistic Binary

@article{Antoniadis2013AMP,
  title={A Massive Pulsar in a Compact Relativistic Binary},
  author={John Antoniadis and Paulo C. C. Freire and Norbert Wex and Thomas M. Tauris and Ryan S. Lynch and Marten H. van Kerkwijk and Michael Kramer and C. G. Bassa and Vik S. Dhillon and Thomas Driebe and Jason W. T. Hessels and Victoria M. Kaspi and Vladislav I. Kondratiev and Norbert Langer and Thomas R. Marsh and Maura Mclaughlin and Timothy T. Pennucci and Scott M. Ransom and Ingrid H. Stairs and Joeri van Leeuwen and Joris P W Verbiest and David G. Whelan},
  journal={Science},
  year={2013},
  volume={340}
}
Introduction Neutron stars with masses above 1.8 solar masses (M☉), possess extreme gravitational fields, which may give rise to phenomena outside general relativity. These strong-field deviations lack experimental confrontation, because they become observable only in tight binaries containing a high-mass pulsar and where orbital decay resulting from emission of gravitational waves can be tested. Understanding the origin of such a system would also help to answer fundamental questions of close… 

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References

SHOWING 1-10 OF 120 REFERENCES

A two-solar-mass neutron star measured using Shapiro delay

Radio timing observations of the binary millisecond pulsar J1614-2230 that show a strong Shapiro delay signature are presented and the pulsar mass is calculated to be (1.97 ± 0.04)M⊙, which rules out almost all currently proposed hyperon or boson condensate equations of state.

Pulsar timing and relativistic gravity

  • J. Taylor
  • Physics
    Philosophical Transactions of the Royal Society of London. Series A: Physical and Engineering Sciences
  • 1992
In addition to being fascinating objects to study in their own right, pulsars are exquisite tools for probing a variety of issues in basic physics. Recycled pulsars, thought to have been spun up in

Strong-field tests of relativistic gravity and binary pulsars.

  • DamourTaylor
  • Physics
    Physical review. D, Particles and fields
  • 1992
A detailed account of the parametrized post-Keplerian'' (PPK) formalism, a general phenomenological framework designed to extract the maximum possible information from pulsar timing and pulse-structure data, and how it can be combined with the predictions of a rather generic class of tensor biscalar theories to bring together tests based on observations of several different pulsars.

THE MASSIVE PULSAR PSR J1614−2230: LINKING QUANTUM CHROMODYNAMICS, GAMMA-RAY BURSTS, AND GRAVITATIONAL WAVE ASTRONOMY

The recent measurement of the Shapiro delay in the radio pulsar PSR J1614−2230 yielded a mass of 1.97 ± 0.04 M☉, making it the most massive pulsar known to date. Its mass is high enough that, even

Studies of the Relativistic Binary Pulsar PSR B1534+12. I. Timing Analysis

We have continued our long-term study of the double neutron star binary pulsar PSR B1534+12, using new instrumentation to make very high precision measurements at the Arecibo Observatory. We have

Formation of Millisecond Pulsars with Heavy White Dwarf Companions: Extreme Mass Transfer on Subthermal Timescales

These systems provide a new formation channel for binary millisecond pulsars with heavy CO white dwarfs and relatively short orbital periods and are concluded that to produce a binary pulsar with a O-Ne-Mg white dwarf or Porb approximately 1 day the above scenario does not work, and a spiral-in phase is still considered the most plausible scenario for the formation of such a system.

Tests of General Relativity from Timing the Double Pulsar

By measuring relativistic corrections to the Keplerian description of the orbital motion, it is found that the “post-Keplerian” parameter s agrees with the value predicted by general relativity within an uncertainty of 0.05%, the most precise test yet obtained.

Collapse of Neutron Stars to Black Holes in Binary Systems: A Model for Short Gamma-Ray Bursts

The accretion of ≈0.1-1 M☉ of material by a neutron star through Roche lobe overflow of its companion or through white dwarf-neutron star coalescence in a low-mass binary system could be enough to

Transformation of a Star into a Planet in a Millisecond Pulsar Binary

This pulsar PSR J1719−1438, a 5.7-millisecond pulsar detected in a recent survey with the Parkes 64-meter radio telescope, is shown to be in a binary system with an orbital period of 2.2 hours.
...