An increased estimate of the merger rate of double neutron stars from observations of a highly relativistic system

  title={An increased estimate of the merger rate of double neutron stars from observations of a highly relativistic system},
  author={Marta Burgay and Nicolo' D'Amico and Andrea Possenti and Richard N. Manchester and Andrew G. Lyne and Bhuwan Joshi and Maura Mclaughlin and Michael Kramer and John M. Sarkissian and F. Camilo and Vicky Kalogera and C. Kim and Duncan R. Lorimer},
The merger of close binary systems containing two neutron stars should produce a burst of gravitational waves, as predicted by the theory of general relativity. A reliable estimate of the double-neutron-star merger rate in the Galaxy is crucial in order to predict whether current gravity wave detectors will be successful in detecting such bursts. Present estimates of this rate are rather low, because we know of only a few double-neutron-star binaries with merger times less than the age of the… 
On the Eccentricities and Merger Rates of Double Neutron Star Binaries and the Creation of “Double Supernovae”
We demonstrate that a natural consequence of an asymmetric kick imparted to neutron stars at birth is that the majority of double neutron star binaries should possess highly eccentric orbits. This
Mergers of Binary Neutron Star Systems: A Multimessenger Revolution
  • E. Pian
  • Physics
    Frontiers in Astronomy and Space Sciences
  • 2020
On August 17, 2017, less than two years after the direct detection of gravitational radiation from the merger of two ∼ 30 M ⊙ black holes, a binary neutron star merger was identified as the source of
The Double Pulsar: Evidence for Neutron Star Formation without an Iron Core-collapse Supernova
The double pulsar system PSR J0737–3039A/B is a double neutron star binary, with a 2.4 hr orbital period, which has allowed measurement of relativistic orbital perturbations to high precision. The
An Upper Bound on Neutron Star Masses from Models of Short Gamma-ray Bursts
The discovery of two neutron stars with gravitational masses $\approx 2~M_\odot$ has placed a strong lower limit on the maximum mass of nonrotating neutron stars, and with it a strong constraint on
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Understanding the nature of galactic populations of double compact binaries (where both stars are a neutron star or black hole) has been a topic of interest for many years, particularly the
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Radio pulsars tend to be high-velocity objects, which implies that the majority of them received a velocity kick of several hundreds of km s(-1) at birth. However, six of the eight known double
The Gravitational waves merger time distribution of binary neutron star systems
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Neutron stars in close binaries with elliptical component orbits
We consider the evolution of close binaries in which the initial secondary component is a nondegenerate helium star with mass MHe = 0.4–60 M⊙, while the initially more massive primary has evolved
We report on the newly increased event rates due to the recent discovery of the highly relativistic binary pulsar J07373039. Using a rigorous statistical method, we present the calculations reported
The double-pulsar binary J0737–3039
Abstract A recent multibeam pulsar survey of the outer Galactic plane at Parkes has discovered the first-known double-pulsar binary, a very compact double neutron star system in which both stars are


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Previous calculations of the merging rate of double neutron star systems similar to the Hulse-Taylor binary pulsar B1913 + 16 have assumed lifetimes based on the sum of the radio pulsar spin-down age
The Rate of Neutron Star Binary Mergers in the Universe: Minimal Predictions for Gravity Wave Detectors
Of the many sources which gravitational wave observatories might see, merging neutron star binaries are the most predictable. Their waveforms at the observable frequencies are easy to calculate. And
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We estimate the coalescence rate of close binaries with two neutron stars (NS) and discuss the prospects for the detection of NS-NS inspiral events by ground-based gravitational-wave observatories,
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There are now about 50 known radio pulsars in binary systems, including at least five in double neutron star binaries. In some cases, the stellar masses can be directly determined from measurements
The Probability Distribution of Binary Pulsar Coalescence Rates. I. Double Neutron Star Systems in the Galactic Field
Estimates of the Galactic coalescence rate () of close binaries with two neutron stars (NS-NS) are known to be uncertain by large factors (about 2 orders of magnitude) mainly because of the small
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From considerations of spin evolution and kinematics in the Galactic potential, we argue that the pulsars B1913+16, B1534+12, and B2127+11C may be younger than previously assumed, and we find that a
Determining the stellar masses in the binary system containing the pulsar PSR 1913 + 16 - Is the companion a helium main-sequence star
The stellar masses and the angle of inclination are determined for the system containing PSR 1913+16 in terms of the observable periastron advance and second-order relativistic effects, for the cases
The binary pulsar: physical processes, possible companions, and evolutionary histories.
A study of some aspects of the binary pulsar, PSR 1913+16, is presented in the light of recently reported observational results. If the companion to the pulsar gives a Newtonian contribution to the
The Probability Distribution of Binary Pulsar Coalescence Rates
Inspiraling binary systems are good candidates for being detected by ground‐based gravitational‐wave detectors. In this work, we present a statistical analysis method to estimate the coalescence rate
Pulsar timing and relativistic gravity
Measurements of the times of arrival of pulsar signals at Earth provide uniquely powerful tools for experiments in relativistic gravity. The results of such experiments improve rapidly as the span of