Using gravitational-wave observations and quasi-universal relations to constrain the maximum mass of neutron stars

@article{Rezzolla2017UsingGO,
  title={Using gravitational-wave observations and quasi-universal relations to constrain the maximum mass of neutron stars},
  author={Luciano Rezzolla and Elias R. Most and Lukas R. Weih},
  journal={arXiv: High Energy Astrophysical Phenomena},
  year={2017}
}
Combining the GW observations of merging systems of binary neutron stars and quasi-universal relations, we set constraints on the maximum mass that can be attained by nonrotating stellar models of neutron stars. More specifically, exploiting the recent observation of the GW event GW 170817 and drawing from basic arguments on kilonova modeling of GRB 170817A, together with the quasi-universal relation between the maximum mass of nonrotating stellar models $M_{\rm TOV}$ and the maximum mass… 

Figures from this paper

What Constraints on the Neutron Star Maximum Mass Can One Pose from GW170817 Observations?
The post-merger product of the first binary neutron star merger event detected in gravitational waves, GW170817, depends on neutron star equation of state (EoS) and is not well determined. We
Total gravitational mass of the Galactic Double Neutron Star systems: evidence for a bimodal distribution
So far, in total 15 double neutron star systems (DNSs) with a reliable measurement of the total gravitational mass ($M_{\rm T}$) have been detected in the Galaxy. In this work we study the
Stringent constraints on neutron-star radii from multimessenger observations and nuclear theory
The properties of neutron stars are determined by the nature of the matter that they contain. These properties can be constrained by measurements of the star’s size. We obtain stringent constraints
Empirical relations for gravitational-wave asteroseismology of binary neutron star mergers
We construct new, multivariate empirical relations for measuring neutron star radii and tidal deformabilities from the dominant gravitational wave frequency in the postmerger phase of binary neutron
The radius of the quiescent neutron star in the globular cluster M13
X-ray spectra of quiescent low-mass X-ray binaries containing neutron stars can be fit with atmosphere models to constrain the mass and the radius. Mass-radius constraints can be used to place limits
The heavier the better: how to constrain mass ratios and spins of high-mass neutron star mergers
The first binary neutron-star merger event, GW170817, and its bright electromagnetic counterpart have provided a remarkable amount of information. By contrast, the second event, GW190425, with
Combined Constraints on the Equation of State of Dense Neutron-rich Matter from Terrestrial Nuclear Experiments and Observations of Neutron Stars
Within the parameter space of equation of state (EOS) of dense neutron-rich matter limited by existing constraints mainly from terrestrial nuclear experiments, we investigate how the neutron star
Relation between gravitational mass and baryonic mass for non-rotating and rapidly rotating neutron stars
With a selected sample of neutron star (NS) equations of state (EOSs) that are consistent with the current observations and have a range of maximum masses, we investigate the relations between NS
Inferring neutron star properties from GW170817 with universal relations
Because all neutron stars share a common equation of state, tidal deformability constraints from the compact binary coalescence GW170817 have implications for the properties of neutron stars in other
Optimal Neutron-star Mass Ranges to Constrain the Equation of State of Nuclear Matter with Electromagnetic and Gravitational-wave Observations
Exploiting a very large library of physically plausible equations of state (EOSs) containing more than $10^{7}$ members and yielding more than $10^{9}$ stellar models, we conduct a survey of the
...
1
2
3
4
5
...

References

SHOWING 1-10 OF 61 REFERENCES
Constraining the Maximum Mass of Neutron Stars from Multi-messenger Observations of GW170817
We combine electromagnetic (EM) and gravitational wave (GW) information on the binary neutron star (NS) merger GW170817 in order to constrain the radii $R_{\rm ns}$ and maximum mass $M_{\rm max}$ of
Rotational properties of hypermassive neutron stars from binary mergers
Determining the differential-rotation law of compact stellar objects produced in binary neutron stars mergers or core-collapse supernovae is an old problem in relativistic astrophysics. Addressing
Measurability of the tidal deformability by gravitational waves from coalescing binary neutron stars
Combining new gravitational waveforms derived by long-term (14--16 orbits) numerical-relativity simulations with waveforms by an effective-one-body (EOB) formalism for coalescing binary neutron
GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral.
TLDR
The association of GRB 170817A, detected by Fermi-GBM 1.7 s after the coalescence, corroborates the hypothesis of a neutron star merger and provides the first direct evidence of a link between these mergers and short γ-ray bursts.
A Neutron Star Binary Merger Model for GW170817/GRB 170817A/SSS17a
The merging neutron star gravitational wave event GW170817 has been observed throughout the entire electromagnetic spectrum from radio waves to $\gamma$-rays. The resulting energetics, variability,
Spectral analysis of gravitational waves from binary neutron star merger remnants
In this work we analyze the gravitational wave signal from hypermassive neutron stars formed after the merger of binary neutron star systems, focusing on its spectral features. The gravitational wave
Gravitational Waves and Gamma-Rays from a Binary Neutron Star Merger: GW170817 and GRB 170817A
On 2017 August 17, the gravitational-wave event GW170817 was observed by the Advanced LIGO and Virgo detectors, and the gamma-ray burst (GRB) GRB 170817A was observed independently by the Fermi
Gravitational-wave signal from binary neutron stars: A systematic analysis of the spectral properties
A number of works have shown that important information on the equation of state of matter at nuclear density can be extracted from the gravitational waves emitted by merging neutron-star binaries.
Spectral properties of the post-merger gravitational-wave signal from binary neutron stars
Extending previous work by a number of authors, we have recently presented a new approach in which the detection of gravitational waves from merging neutron star binaries can be used to determine the
The Neutron star and black hole initial mass function
Using recently calculated models for massive stellar evolution and supernovae coupled to a model for Galactic chemical evolution, neutron star and black hole birth functions (number of neutron stars
...
1
2
3
4
5
...