--- CQMC model within relativistic Hartree-Fock approximation and Thomas-Fermi model ---

This web site provides equation of state (EOS) for neutron star matter. The chiral quark-meson coupling (CQMC) model within relativistic Hartree-Fock approximation is adopted for uniform nuclear matter. All octet baryons are considered in the core region, while onlyΞappears in neutron stars. In the crust region, nuclei are taken into account within the Thomas-Fermi calculation. For the details, see Miyatsu et al. (2013), arXiv:1308.6121 [astro-ph.HE]. This EOS table is open for general use in any numerical simulations for astrophysics, provided that our paper is referenced in your publication.^{-}

- guide.pdf (55.7kB)

- Baryon mass density, energy density, pressure and lepton (= electron + muon) fraction (26.8kB)
- Particle fractions (68.8kB)
- Properties of nuclei in the crust region (13.1kB)

- Saturation density: 0.155 fm
^{-3} - Saturation energy: -16.1 MeV
- Symmetry energy: 33.6 MeV (32.7 MeV)
- Slope of symmetry energy: 77.1 MeV (75.8 MeV)
- Incompressibility: 274 MeV
- Maximum mass of neutron star: 1.95
*M*_{solar}

Note: There are two diffinitions of symmetry energy. See Section 3.2 and Table 2 of our paper for the details.

- Tsuyoshi Miyatsu
- Department of Physics, Soongsil University
- Seoul 156-743, Korea
- E-mail: tmiyatsu@ssu.ac.kr

- Ken'ichiro Nakazato
- Department of Physics, Faculty of Science & Technology, Tokyo University of Science
- 2641 Yamazaki, Noda, Chiba 278-8510, Japan
- E-mail: nakazato@rs.tus.ac.jp

Please reference the following paper when you publish scientific articles using this EOS.

- A new equation of state for neutron star matter with nuclei in the crust and hyperons in the core,

T. Miyatsu, S. Yamamuro, and K. Nakazato,

arXiv:1308.6121 [astro-ph.HE]

Last up date, Aug. 29, 2013.