Binary neutron star mergers: Dependence on the nuclear equation of state

@article{Hotokezaka2011BinaryNS,
  title={Binary neutron star mergers: Dependence on the nuclear equation of state},
  author={Kenta Hotokezaka and Koutarou Kyutoku and Hirotada Okawa and Masaru Shibata and Kenta Kiuchi},
  journal={Physical Review D},
  year={2011},
  volume={83},
  pages={124008}
}
We perform a numerical-relativity simulation for the merger of binary neutron stars with 6 nuclear-theory-based equations of states (EOSs) described by piecewise polytropes. Our purpose is to explore the dependence of the dynamical behavior of the binary neutron star merger and resulting gravitational waveforms on the EOS of the supernuclear-density matter. The numerical results show that the merger process and the first outcome are classified into three types: (i) a black hole is promptly… 

Figures and Tables from this paper

Mass ejection from the merger of binary neutron stars
Numerical-relativity simulations for the merger of binary neutron stars are performed for a variety of equations of state (EOSs) and for a plausible range of the neutron-star mass, focusing primarily
Binary Neutron Star Mergers: Mass Ejection, Electromagnetic Counterparts, and Nucleosynthesis
We present a systematic numerical relativity study of the mass ejection and the associated electromagnetic transients and nucleosynthesis from binary neutron star (NS) mergers. We find that a few
Binary Neutron Star Mergers
TLDR
The quasi-equilibrium approximation has played a key role in developing understanding of the physics of binary coalescence and, in particular, of the orbital instability processes that can drive binaries to merger at the end of their lifetimes.
Neutrino-driven winds in the aftermath of a neutron star merger: nucleosynthesis and electromagnetic transients
We present a comprehensive nucleosynthesis study of the neutrino-driven wind in the aftermath of a binary neutron star merger. Our focus is the initial remnant phase when a massive central neutron
Gravitational waves and neutrino emission from the merger of binary neutron stars.
TLDR
The neutrino luminosity curve when a black hole is formed for the first time is presented and the effective amplitude of gravitational waves from the HMNS is 4-6×10(-22) at f=2.1-2.5  kHz.
Accretion-induced prompt black hole formation in asymmetric neutron star mergers, dynamical ejecta, and kilonova signals
We present new numerical relativity results of neutron star mergers with chirp mass $1.188M_\odot$ and mass ratios $q=1.67$ and $q=1.8$ using finite-temperature equations of state (EOS), approximate
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
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
Gravitational waves, neutrino emissions, and effects of hyperons in binary neutron star mergers
Numerical simulations for the merger of binary neutron stars are performed in full general relativity incorporating both nucleonic and hyperonic finite-temperature equations of state (EOS) and
Exploring properties of high-density matter through remnants of neutron-star mergers
Abstract.Remnants of neutron-star mergers are essentially massive, hot, differentially rotating neutron stars, which are initially strongly oscillating. As such they represent a unique probe for
...
...

References

SHOWING 1-10 OF 31 REFERENCES
Phys
  • 160, 241
  • 2000
Class
Phys
  • Rev. D 63, 064029
  • 2001
Phys
  • Rev. D 59, 024007
  • 1998
Astrophys
  • J. 629, 969
  • 2005
submitted to Phys
  • Rev. Lett.
  • 2011
Astrophys
  • J. Suppl. 188, 187
  • 2010
Phys
  • Rev. D 52, 5428
  • 1995
Astrophys
  • J. 398, 234
  • 1992
Phys
  • Rev. D 68, 084020
  • 2003
...
...