Bayesian Inference of Strange Star Equation of State Using the GW170817 and GW190425 Data

@article{Miao2021BayesianIO,
  title={Bayesian Inference of Strange Star Equation of State Using the GW170817 and GW190425 Data},
  author={Zhiqiang Miao and Jin-Liang Jiang and Ang Li and Lie-Wen Chen},
  journal={The Astrophysical Journal Letters},
  year={2021},
  volume={917}
}
The observations of compact star inspirals from LIGO/Virgo provide a valuable tool to study the highly uncertain equation of state (EOS) of dense matter at the densities in which the compact stars reside. It is not clear whether the merging stars are neutron stars or quark stars containing self-bound quark matter. In this work, we explore the allowed bag-model-like EOSs by assuming the merging stars are strange quark stars (SQSs) from a Bayesian analysis employing the tidal deformability… 
5 Citations

References

SHOWING 1-10 OF 95 REFERENCES

Was GW190814 a Black Hole-Strange Quark Star System?

TLDR
It is investigated the possibility that the low mass companion of the black hole in the source of GW190814 was a strange quark star, which could fulfill the presently available astrophysical and nuclear physics constraints which require a softer equation of state.

Constraints on the Maximum Mass of Neutron Stars with a Quark Core from GW170817 and NICER PSR J0030+0451 Data

We perform a Bayesian analysis of the maximum mass M TOV of neutron stars with a quark core, incorporating the observational data from tidal deformability of the GW170817 binary neutron star merger

GW170817: Measurements of Neutron Star Radii and Equation of State.

TLDR
This analysis expands upon previous analyses by working under the hypothesis that both bodies were neutron stars that are described by the same equation of state and have spins within the range observed in Galactic binary neutron stars.

Bayesian inference of quark star equation of state using the NICER PSR J0030+0451 data

We constrain the equation of state of quark stars within the Bayesian statistical approach using the mass and radius measurements of PSR J0030+0451 from NICER. Three types of bag models, with and

Sound velocity in dense stellar matter with strangeness and compact stars *

The phase state in the intermediate density range of dense matter ($\sim1-10$ times of nuclear saturation density) is both intriguing and unclear, and could have important observable effects in the

Neutron Skins and Neutron Stars in the Multimessenger Era.

TLDR
A set of realistic models of the equation of state (EOS) that yield an accurate description of the properties of finite nuclei, support neutron stars of two solar masses, and provide a Lorentz covariant extrapolation to dense matter are used to confront its predictions against tidal polarizabilities extracted from the gravitational-wave data.

Critical examination of constraints on the equation of state of dense matter obtained from GW170817

The correlation of the tidal polarizabilities Λ1-Λ2 for GW170817 is predicted by combining dense-matter equations of state (EOSs) that satisfy nuclear physics constraints with the chirp mass and mass

Constraining the Neutron Star Equation of State Using Multiband Independent Measurements of Radii and Tidal Deformabilities.

Using a Bayesian approach, we combine measurements of neutron star macroscopic observables obtained by astrophysical and gravitational observations to derive joint constraints on the equation of

PSR J0030+0451 Mass and Radius from NICER Data and Implications for the Properties of Neutron Star Matter

Neutron stars are not only of astrophysical interest, but are also of great interest to nuclear physicists because their attributes can be used to determine the properties of the dense matter in
...