Simulating Binary Neutron Stars with Hybrid Equation of States: Gravitational Waves, Electromagnetic Signatures and Challenges for Numerical Relativity
Abstract
:1. Introduction
2. A New Hybrid Star Equation of State
2.1. tdBag Model for Strange Quark Matter
- The quartic coefficient can be interpreted as a correction to the pressure of the free Fermi sea arising from quantum chromodynamics (QCD). Fraga et al. [41] show that, to second order in the strong coupling constant, a reasonable value for this parameter is . The values of and correspond to maximum or none QCD interaction, respectively.
- The bag constant B, introduced phenomenologically into the theory to describe the deconfinement, is the energy density required to produce a “vacuumless” volume in which quarks exist.
- The contribution of the electron potential () for our purposes is negligible; cf. Reference [43] and references therein. Nevertheless, if the SQM is not in the CFL phase [40] there must be electrons within the quark phase to ensure (i) local charge neutrality and (ii) chemical equilibrium. These two conditions may be expressed respectively as
2.2. Thermodynamics and Parameter Analysis
- (i)
- : not allowed region due to the fact that hadronic matter is more stable than quark matter, then we cannot use a SQM EoS.
- (ii)
- : absolutely stable strange stars (SS). There is no phase transition HM → SQM and the star is entirely made of 3-flavor quarks.
- (iii)
- : HyS. There exists a phase transition between HM and SQM for some energy density .
- (i)
- : HM EoS,
- (ii)
- : ,
- (iii)
- : SQM EoS.
2.3. Building Hybrid Star EoS
2.4. HyS EoS as Piecewise Polytropes
3. Configurations Details and Numerical Methods
3.1. Hybrid Star Configuration
3.2. Numerical Methods
4. Quantitative Merger Dynamics
5. Gravitational Wave Signal
5.1. The Inspiral
5.2. The Postmerger
6. Ejecta and Electromagnetic Counterparts
7. Conclusions
Author Contributions
Funding
Acknowledgments
Conflicts of Interest
Abbreviations
BH | Black Hole |
BNS | Binary Neutron Star |
CFL | Color-flavor-locked |
EM | Electromagnetic |
EoS | Equation of State |
GRB | Gamma Ray Burst |
GRHD | General Relativistic Hydrodynamics |
GW | Gravitational Wave |
HM | Hadronic Matter |
HRSC | High-resolution Shock-capturing |
HyS | Hybrid Star |
LLF | Local Lax-Friedrich |
MIT | Massachusetts Institute of Technology |
NR | Numerical Relativity |
NS | Neutron Star |
QCD | Quantum Chromodynamics |
SQM | Strange Quark Matter |
WENOZ | Weighted Essentially Non-oscillatory |
Appendix A. HyS Piecewise Polytrope
K | ||
---|---|---|
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e | |||||||
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1.365 | 1.527 | 0.18 | 11.0 | 378 | 2.705 | 8.324 |
Name | n | ||||
---|---|---|---|---|---|
R1 | 4 | 192 | 64 | ||
R2 | 4 | 288 | 96 | ||
R3 | 4 | 384 | 128 | ||
R4 | 4 | 480 | 160 |
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Gieg, H.; Dietrich, T.; Ujevic, M. Simulating Binary Neutron Stars with Hybrid Equation of States: Gravitational Waves, Electromagnetic Signatures and Challenges for Numerical Relativity. Particles 2019, 2, 365-384. https://doi.org/10.3390/particles2030023
Gieg H, Dietrich T, Ujevic M. Simulating Binary Neutron Stars with Hybrid Equation of States: Gravitational Waves, Electromagnetic Signatures and Challenges for Numerical Relativity. Particles. 2019; 2(3):365-384. https://doi.org/10.3390/particles2030023
Chicago/Turabian StyleGieg, Henrique, Tim Dietrich, and Maximiliano Ujevic. 2019. "Simulating Binary Neutron Stars with Hybrid Equation of States: Gravitational Waves, Electromagnetic Signatures and Challenges for Numerical Relativity" Particles 2, no. 3: 365-384. https://doi.org/10.3390/particles2030023